Search | arXiv e-print repository

<!DOCTYPE html> <html lang="en"> <head> <meta charset="utf-8"/> <meta name="viewport" content="width=device-width, initial-scale=1"/>  <link rel="apple-touch-icon" sizes="180x180" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/apple-touch-icon.png"> <link rel="icon" type="image/png" sizes="32x32" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon-32x32.png"> <link rel="icon" type="image/png" sizes="16x16" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon-16x16.png"> <link rel="manifest" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/site.webmanifest"> <link rel="mask-icon" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/safari-pinned-tab.svg" color="#b31b1b"> <link rel="shortcut icon" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon.ico"> <meta name="msapplication-TileColor" content="#b31b1b"> <meta name="msapplication-config" content="images/icons/browserconfig.xml"> <meta name="theme-color" content="#b31b1b">  <title>Search | arXiv e-print repository</title> <script defer src="https://static.arxiv.org/static/base/1.0.0a5/fontawesome-free-5.11.2-web/js/all.js"></script> <link rel="stylesheet" href="https://static.arxiv.org/static/base/1.0.0a5/css/arxivstyle.css" /> <script type="text/x-mathjax-config"> MathJax.Hub.Config({ messageStyle: "none", extensions: ["tex2jax.js"], jax: ["input/TeX", "output/HTML-CSS"], tex2jax: { inlineMath: [ ['$','$'], ["\$","\$"] ], displayMath: [ ['$$','$$'], ["\\[","\\]"] ], processEscapes: true, ignoreClass: '.*', processClass: 'mathjax.*' }, TeX: { extensions: ["AMSmath.js", "AMSsymbols.js", "noErrors.js"], noErrors: { inlineDelimiters: ["$","$"], multiLine: false, style: { "font-size": "normal", "border": "" } } }, "HTML-CSS": { availableFonts: ["TeX"] } }); </script> <script src='//static.arxiv.org/MathJax-2.7.3/MathJax.js'></script> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/notification.js"></script> <link rel="stylesheet" href="https://static.arxiv.org/static/search/0.5.6/css/bulma-tooltip.min.css" /> <link rel="stylesheet" href="https://static.arxiv.org/static/search/0.5.6/css/search.css" /> <script src="https://code.jquery.com/jquery-3.2.1.slim.min.js" integrity="sha256-k2WSCIexGzOj3Euiig+TlR8gA0EmPjuc79OEeY5L45g=" crossorigin="anonymous"></script> <script src="https://static.arxiv.org/static/search/0.5.6/js/fieldset.js"></script> <style> radio#cf-customfield_11400 { display: none; } </style> </head> <body> <header><a href="#main-container" class="is-sr-only">Skip to main content</a>  <div class="attribution level is-marginless" role="banner"> <div class="level-left"> <a class="level-item" href="https://cornell.edu/"><img src="https://static.arxiv.org/static/base/1.0.0a5/images/cornell-reduced-white-SMALL.svg" alt="Cornell University" width="200" aria-label="logo" /></a> </div> <div class="level-right is-marginless"><p class="sponsors level-item is-marginless"><span id="support-ack-url">We gratefully acknowledge support from<br /> the Simons Foundation, <a href="https://info.arxiv.org/about/ourmembers.html">member institutions</a>, and all contributors. <a href="https://info.arxiv.org/about/donate.html">Donate</a></span></p></div> </div>  <div class="identity level is-marginless"> <div class="level-left"> <div class="level-item"> <a class="arxiv" href="https://arxiv.org/" aria-label="arxiv-logo"> <img src="https://static.arxiv.org/static/base/1.0.0a5/images/arxiv-logo-one-color-white.svg" aria-label="logo" alt="arxiv logo" width="85" style="width:85px;"/> </a> </div> </div> <div class="search-block level-right"> <form class="level-item mini-search" method="GET" action="https://arxiv.org/search"> <div class="field has-addons"> <div class="control"> <input class="input is-small" type="text" name="query" placeholder="Search..." aria-label="Search term or terms" /> <p class="help"><a href="https://info.arxiv.org/help">Help</a> | <a href="https://arxiv.org/search/advanced">Advanced Search</a></p> </div> <div class="control"> <div class="select is-small"> <select name="searchtype" aria-label="Field to search"> <option value="all" selected="selected">All fields</option> <option value="title">Title</option> <option value="author">Author</option> <option value="abstract">Abstract</option> <option value="comments">Comments</option> <option value="journal_ref">Journal reference</option> <option value="acm_class">ACM classification</option> <option value="msc_class">MSC classification</option> <option value="report_num">Report number</option> <option value="paper_id">arXiv identifier</option> <option value="doi">DOI</option> <option value="orcid">ORCID</option> <option value="author_id">arXiv author ID</option> <option value="help">Help pages</option> <option value="full_text">Full text</option> </select> </div> </div> <input type="hidden" name="source" value="header"> <button class="button is-small is-cul-darker">Search</button> </div> </form> </div> </div>  <div class="container"> <div class="user-tools is-size-7 has-text-right has-text-weight-bold" role="navigation" aria-label="User menu"> <a href="https://arxiv.org/login">Login</a> </div> </div> </header> <main class="container" id="main-container"> <div class="level is-marginless"> <div class="level-left"> <h1 class="title is-clearfix"> Showing 1–50 of 128 results for author: <span class="mathjax">Carry, B</span> </h1> </div> <div class="level-right is-hidden-mobile">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> <div class="content"> <form method="GET" action="/search/astro-ph" aria-role="search"> Searching in archive <strong>astro-ph</strong>. <a href="/search/?searchtype=author&query=Carry%2C+B">Search in all archives.</a> <div class="field has-addons-tablet"> <div class="control is-expanded"> <label for="query" class="hidden-label">Search term or terms</label> <input class="input is-medium" id="query" name="query" placeholder="Search term..." type="text" value="Carry, B"> </div> <div class="select control is-medium"> <label class="is-hidden" for="searchtype">Field</label> <select class="is-medium" id="searchtype" name="searchtype"><option value="all">All fields</option><option value="title">Title</option><option selected value="author">Author(s)</option><option value="abstract">Abstract</option><option value="comments">Comments</option><option value="journal_ref">Journal reference</option><option value="acm_class">ACM classification</option><option value="msc_class">MSC classification</option><option value="report_num">Report number</option><option value="paper_id">arXiv identifier</option><option value="doi">DOI</option><option value="orcid">ORCID</option><option value="license">License (URI)</option><option value="author_id">arXiv author ID</option><option value="help">Help pages</option><option value="full_text">Full text</option></select> </div> <div class="control"> <button class="button is-link is-medium">Search</button> </div> </div> <div class="field"> <div class="control is-size-7"> <label class="radio"> <input checked id="abstracts-0" name="abstracts" type="radio" value="show"> Show abstracts </label> <label class="radio"> <input id="abstracts-1" name="abstracts" type="radio" value="hide"> Hide abstracts </label> </div> </div> <div class="is-clearfix" style="height: 2.5em"> <div class="is-pulled-right"> <a href="/search/advanced?terms-0-term=Carry%2C+B&terms-0-field=author&size=50&order=-announced_date_first">Advanced Search</a> </div> </div> <input type="hidden" name="order" value="-announced_date_first"> <input type="hidden" name="size" value="50"> </form> <div class="level breathe-horizontal"> <div class="level-left"> <form method="GET" action="/search/"> <div style="display: none;"> <select id="searchtype" name="searchtype"><option value="all">All fields</option><option value="title">Title</option><option selected value="author">Author(s)</option><option value="abstract">Abstract</option><option value="comments">Comments</option><option value="journal_ref">Journal reference</option><option value="acm_class">ACM classification</option><option value="msc_class">MSC classification</option><option value="report_num">Report number</option><option value="paper_id">arXiv identifier</option><option value="doi">DOI</option><option value="orcid">ORCID</option><option value="license">License (URI)</option><option value="author_id">arXiv author ID</option><option value="help">Help pages</option><option value="full_text">Full text</option></select> <input id="query" name="query" type="text" value="Carry, B"> <ul id="abstracts"><li><input checked id="abstracts-0" name="abstracts" type="radio" value="show"> <label for="abstracts-0">Show abstracts</label></li><li><input id="abstracts-1" name="abstracts" type="radio" value="hide"> <label for="abstracts-1">Hide abstracts</label></li></ul> </div> <div class="box field is-grouped is-grouped-multiline level-item"> <div class="control"> <span class="select is-small"> <select id="size" name="size"><option value="25">25</option><option selected value="50">50</option><option value="100">100</option><option value="200">200</option></select> </span> <label for="size">results per page</label>. </div> <div class="control"> <label for="order">Sort results by</label> <span class="select is-small"> <select id="order" name="order"><option selected value="-announced_date_first">Announcement date (newest first)</option><option value="announced_date_first">Announcement date (oldest first)</option><option value="-submitted_date">Submission date (newest first)</option><option value="submitted_date">Submission date (oldest first)</option><option value="">Relevance</option></select> </span> </div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Carry%2C+B&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Carry%2C+B&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Carry%2C+B&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Carry%2C+B&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.08585">arXiv:2410.08585</a> <span> [<a href="https://arxiv.org/pdf/2410.08585">pdf</a>, <a href="https://arxiv.org/format/2410.08585">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Signal Processing">eess.SP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.3019874">10.1117/12.3019874 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Blind and robust reconstruction of adaptive optics point spread functions for asteroid deconvolution and moon detection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Berdeu%2C+A">Anthony Berdeu</a>, <a href="/search/astro-ph?searchtype=author&query=Soulez%2C+F">F茅rr茅ol Soulez</a>, <a href="/search/astro-ph?searchtype=author&query=Minker%2C+K">Kate Minker</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Bourdarot%2C+G">Guillaume Bourdarot</a>, <a href="/search/astro-ph?searchtype=author&query=Kaszczyc%2C+A">Antoine Kaszczyc</a>, <a href="/search/astro-ph?searchtype=author&query=Langlois%2C+M">Maud Langlois</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.08585v1-abstract-short" style="display: inline;"> Initially designed to detect and characterize exoplanets, extreme adaptive optics systems (AO) open a new window on the solar system by resolving its small bodies. Nonetheless, despite the always increasing performances of AO systems, the correction is not perfect, degrading their image and producing a bright halo that can hide faint and close moons. Using a reference point spread function (PSF) i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.08585v1-abstract-full').style.display = 'inline'; document.getElementById('2410.08585v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.08585v1-abstract-full" style="display: none;"> Initially designed to detect and characterize exoplanets, extreme adaptive optics systems (AO) open a new window on the solar system by resolving its small bodies. Nonetheless, despite the always increasing performances of AO systems, the correction is not perfect, degrading their image and producing a bright halo that can hide faint and close moons. Using a reference point spread function (PSF) is not always sufficient due to the random nature of the turbulence. In this work, we present our method to overcome this limitation. It blindly reconstructs the AO-PSF directly in the data of interest, without any prior on the instrument nor the asteroid's shape. This is done by first estimating the PSF core parameters under the assumption of a sharp-edge and flat object, allowing the image of the main body to be deconvolved. Then, the PSF faint extensions are reconstructed with a robust penalization optimization, discarding outliers on-the-fly such as cosmic rays, defective pixels and moons. This allows to properly model and remove the asteroid's halo. Finally, moons can be detected in the residuals, using the reconstructed PSF and the knowledge of the outliers learned with the robust method. We show that our method can be easily applied to different instruments (VLT/SPHERE, Keck/NIRC2), efficiently retrieving the features of AO-PSFs. Compared with state-of-the-art moon enhancement algorithms, moon signal is greatly improved and our robust detection method manages to discriminate faint moons from outliers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.08585v1-abstract-full').style.display = 'none'; document.getElementById('2410.08585v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">arXiv admin note: text overlap with arXiv:2407.21548</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Adaptive Optics Systems IX, Jun 2024, Yokohama, Japan. pp.235 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.07195">arXiv:2406.07195</a> <span> [<a href="https://arxiv.org/pdf/2406.07195">pdf</a>, <a href="https://arxiv.org/format/2406.07195">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> </div> </div> <p class="title is-5 mathjax"> Binary asteroid candidates in Gaia DR3 astrometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liberato%2C+L">Luana Liberato</a>, <a href="/search/astro-ph?searchtype=author&query=Tanga%2C+P">Paolo Tanga</a>, <a href="/search/astro-ph?searchtype=author&query=Mary%2C+D">David Mary</a>, <a href="/search/astro-ph?searchtype=author&query=Minker%2C+K">Kate Minker</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Spoto%2C+F">Federica Spoto</a>, <a href="/search/astro-ph?searchtype=author&query=Bartczak%2C+P">Przemyslaw Bartczak</a>, <a href="/search/astro-ph?searchtype=author&query=Sicardy%2C+B">Bruno Sicardy</a>, <a href="/search/astro-ph?searchtype=author&query=Oszkiewicz%2C+D">Dagmara Oszkiewicz</a>, <a href="/search/astro-ph?searchtype=author&query=Desmars%2C+J">Josselin Desmars</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.07195v2-abstract-short" style="display: inline;"> Asteroids with companions constitute an excellent sample for studying the collisional and dynamical evolution of minor planets. The currently known binary population were discovered by different complementary techniques that produce, for the moment, a strongly biased distribution, especially in a range of intermediate asteroid sizes (approximately 20 to 100 km) where both mutual photometric events… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07195v2-abstract-full').style.display = 'inline'; document.getElementById('2406.07195v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.07195v2-abstract-full" style="display: none;"> Asteroids with companions constitute an excellent sample for studying the collisional and dynamical evolution of minor planets. The currently known binary population were discovered by different complementary techniques that produce, for the moment, a strongly biased distribution, especially in a range of intermediate asteroid sizes (approximately 20 to 100 km) where both mutual photometric events and high-resolution adaptive optic imaging are poorly efficient. A totally independent technique of binary asteroid discovery, based on astrometry, can help to reveal new binary systems and populate a range of sizes and separations that remain nearly unexplored. In this work, we describe a dedicated period detection method and its results for the Gaia DR3 data set. This method looks for the presence of a periodic signature in the orbit post-fit residuals. After conservative filtering and validation based on statistical and physical criteria, we are able to present a first sample of astrometric binary candidates, to be confirmed by other observation techniques such as photometric light curves and stellar occultations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07195v2-abstract-full').style.display = 'none'; document.getElementById('2406.07195v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 29 figures, Online table currently available at https://lagrange.oca.eu/fr/gaiamoons</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.18460">arXiv:2405.18460</a> <span> [<a href="https://arxiv.org/pdf/2405.18460">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449502">10.1051/0004-6361/202449502 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Binary craters on Ceres and Vesta and implications for binary asteroids </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Herrera%2C+C">Carianna Herrera</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Lagain%2C+A">Anthony Lagain</a>, <a href="/search/astro-ph?searchtype=author&query=Vavilov%2C+D+E">Dmitrii E. Vavilov</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.18460v1-abstract-short" style="display: inline;"> Context. Airless planetary objects have their surfaces covered by craters, and these can be used to study the characteristics of asteroid populations. Planetary surfaces present binary craters that are associated with the synchronous impact of binary asteroids. Aims. We identify binary craters on asteroids (1) Ceres and (4) Vesta, and aim to characterize the properties (size ratio and orbital plan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18460v1-abstract-full').style.display = 'inline'; document.getElementById('2405.18460v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.18460v1-abstract-full" style="display: none;"> Context. Airless planetary objects have their surfaces covered by craters, and these can be used to study the characteristics of asteroid populations. Planetary surfaces present binary craters that are associated with the synchronous impact of binary asteroids. Aims. We identify binary craters on asteroids (1) Ceres and (4) Vesta, and aim to characterize the properties (size ratio and orbital plane) of the binary asteroids that might have formed them. Methods. We used global crater databases developed in previous studies and mosaics of images from the NASA DAWN mission high-altitude and low-altitude mapping orbits. We established selection criteria to identify craters that were most likely a product of the impact of a binary asteroid. We performed numerical simulations to predict the orientation of the binary craters assuming the population of impactors has mutual orbits coplanar with heliocentric orbits, as the current census of binary asteroids suggests. We compared our simulations with our survey of binary craters on Ceres and Vesta through a Kolmogorov-Smirnov test. Results. We find geomorphological evidence of 39 and 18 synchronous impacts on the surfaces of Ceres and Vesta, respectively. The associated binary asteroids are widely separated and similar in diameter. The distributions of the orientation of these binary craters on both bodies are statistically different from numerical impact simulations that assume binary asteroids with coplanar mutual and heliocentric orbits. Conclusions. Although the identification of binary craters on both bodies and the sample size are limited, these findings are consistent with a population of well-separated and similarly sized binary asteroids with nonzero obliquity that remains to be observed, in agreement with the population of binary craters identified on Mars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18460v1-abstract-full').style.display = 'none'; document.getElementById('2405.18460v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 5 figures, 5 tables (1 in main text and 4 in appendix)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 688, A176 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13491">arXiv:2405.13491</a> <span> [<a href="https://arxiv.org/pdf/2405.13491">pdf</a>, <a href="https://arxiv.org/format/2405.13491">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Euclid. I. Overview of the Euclid mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Mellier%2C+Y">Y. Mellier</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Barroso%2C+J+A+A">J. A. Acevedo Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Ach%C3%BAcarro%2C+A">A. Ach煤carro</a>, <a href="/search/astro-ph?searchtype=author&query=Adamek%2C+J">J. Adamek</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Addison%2C+G+E">G. E. Addison</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Ajani%2C+V">V. Ajani</a>, <a href="/search/astro-ph?searchtype=author&query=Akrami%2C+Y">Y. Akrami</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Bahlawan%2C+A">A. Al-Bahlawan</a>, <a href="/search/astro-ph?searchtype=author&query=Alavi%2C+A">A. Alavi</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+S">I. S. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Alestas%2C+G">G. Alestas</a>, <a href="/search/astro-ph?searchtype=author&query=Alguero%2C+G">G. Alguero</a>, <a href="/search/astro-ph?searchtype=author&query=Allaoui%2C+A">A. Allaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+S+W">S. W. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allevato%2C+V">V. Allevato</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Tetilla%2C+A+V">A. V. Alonso-Tetilla</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Candal%2C+A">A. Alvarez-Candal</a>, <a href="/search/astro-ph?searchtype=author&query=Alvi%2C+S">S. Alvi</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a> , et al. (1115 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.13491v2-abstract-short" style="display: inline;"> The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. Euclid is a medium-class mission in the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13491v2-abstract-full').style.display = 'inline'; document.getElementById('2405.13491v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13491v2-abstract-full" style="display: none;"> The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. Euclid is a medium-class mission in the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14,000 deg^2 of extragalactic sky. In addition to accurate weak lensing and clustering measurements that probe structure formation over half of the age of the Universe, its primary probes for cosmology, these exquisite data will enable a wide range of science. This paper provides a high-level overview of the mission, summarising the survey characteristics, the various data-processing steps, and data products. We also highlight the main science objectives and expected performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13491v2-abstract-full').style.display = 'none'; document.getElementById('2405.13491v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the A&A special issue`Euclid on Sky'</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.10486">arXiv:2404.10486</a> <span> [<a href="https://arxiv.org/pdf/2404.10486">pdf</a>, <a href="https://arxiv.org/format/2404.10486">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449763">10.1051/0004-6361/202449763 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a dormant 33 solar-mass black hole in pre-release Gaia astrometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Panuzzo%2C+P">P. Panuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Mazeh%2C+T">T. Mazeh</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</a>, <a href="/search/astro-ph?searchtype=author&query=Caffau%2C+E">E. Caffau</a>, <a href="/search/astro-ph?searchtype=author&query=Jorissen%2C+A">A. Jorissen</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Gavras%2C+P">P. Gavras</a>, <a href="/search/astro-ph?searchtype=author&query=Sahlmann%2C+J">J. Sahlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+U">U. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+%C5%81">艁. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Leclerc%2C+N">N. Leclerc</a>, <a href="/search/astro-ph?searchtype=author&query=Bauchet%2C+N">N. Bauchet</a>, <a href="/search/astro-ph?searchtype=author&query=Bombrun%2C+A">A. Bombrun</a>, <a href="/search/astro-ph?searchtype=author&query=Mowlavi%2C+N">N. Mowlavi</a>, <a href="/search/astro-ph?searchtype=author&query=Seabroke%2C+G+M">G. M. Seabroke</a>, <a href="/search/astro-ph?searchtype=author&query=Teyssier%2C+D">D. Teyssier</a>, <a href="/search/astro-ph?searchtype=author&query=Balbinot%2C+E">E. Balbinot</a>, <a href="/search/astro-ph?searchtype=author&query=Helmi%2C+A">A. Helmi</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a> , et al. (390 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.10486v2-abstract-short" style="display: inline;"> Gravitational waves from black-hole merging events have revealed a population of extra-galactic BHs residing in short-period binaries with masses that are higher than expected based on most stellar evolution models - and also higher than known stellar-origin black holes in our Galaxy. It has been proposed that those high-mass BHs are the remnants of massive metal-poor stars. Gaia astrometry is exp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10486v2-abstract-full').style.display = 'inline'; document.getElementById('2404.10486v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.10486v2-abstract-full" style="display: none;"> Gravitational waves from black-hole merging events have revealed a population of extra-galactic BHs residing in short-period binaries with masses that are higher than expected based on most stellar evolution models - and also higher than known stellar-origin black holes in our Galaxy. It has been proposed that those high-mass BHs are the remnants of massive metal-poor stars. Gaia astrometry is expected to uncover many Galactic wide-binary systems containing dormant BHs, which may not have been detected before. The study of this population will provide new information on the BH-mass distribution in binaries and shed light on their formation mechanisms and progenitors. As part of the validation efforts in preparation for the fourth Gaia data release (DR4), we analysed the preliminary astrometric binary solutions, obtained by the Gaia Non-Single Star pipeline, to verify their significance and to minimise false-detection rates in high-mass-function orbital solutions. The astrometric binary solution of one source, Gaia BH3, implies the presence of a 32.70 \pm 0.82 M\odot BH in a binary system with a period of 11.6 yr. Gaia radial velocities independently validate the astrometric orbit. Broad-band photometric and spectroscopic data show that the visible component is an old, very metal-poor giant of the Galactic halo, at a distance of 590 pc. The BH in the Gaia BH3 system is more massive than any other Galactic stellar-origin BH known thus far. The low metallicity of the star companion supports the scenario that metal-poor massive stars are progenitors of the high-mass BHs detected by gravitational-wave telescopes. The Galactic orbit of the system and its metallicity indicate that it might belong to the Sequoia halo substructure. Alternatively, and more plausibly, it could belong to the ED-2 stream, which likely originated from a globular cluster that had been disrupted by the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10486v2-abstract-full').style.display = 'none'; document.getElementById('2404.10486v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, accepted fro publication in A&A Letters. New version with small fixes</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.20179">arXiv:2403.20179</a> <span> [<a href="https://arxiv.org/pdf/2403.20179">pdf</a>, <a href="https://arxiv.org/format/2403.20179">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449789">10.1051/0004-6361/202449789 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Combined spin orientation and phase function of asteroids </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Peloton%2C+J">J. Peloton</a>, <a href="/search/astro-ph?searchtype=author&query=Montagner%2C+R+L">R. Le Montagner</a>, <a href="/search/astro-ph?searchtype=author&query=Mahlke%2C+M">M. Mahlke</a>, <a href="/search/astro-ph?searchtype=author&query=Berthier%2C+J">J. Berthier</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.20179v1-abstract-short" style="display: inline;"> Large surveys provide numerous non-targeted observations of small bodies (SSOs). The upcoming LSST of the Rubin observatory will be the largest source of SSO photometry in the next decade. With non-coordinated epochs of observation, colors, and therefore taxonomy and composition, can only be computed by comparing absolute magnitudes obtained in each filter by solving the phase function (evolution… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.20179v1-abstract-full').style.display = 'inline'; document.getElementById('2403.20179v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.20179v1-abstract-full" style="display: none;"> Large surveys provide numerous non-targeted observations of small bodies (SSOs). The upcoming LSST of the Rubin observatory will be the largest source of SSO photometry in the next decade. With non-coordinated epochs of observation, colors, and therefore taxonomy and composition, can only be computed by comparing absolute magnitudes obtained in each filter by solving the phase function (evolution of brightness of the small body against the solar phase angle). Current models in use in the community (HG, HG12* , HG1G2) however fail to reproduce the long-term photometry of many targets due to the change in aspect angle between apparitions. We aim at deriving a generic yet simple phase function model accounting for the variable geometry of the SSOs over multiple apparitions. We propose the sHG1G2 phase function model in which we introduce a term describing the brightness changes due to spin orientation and polar oblateness. We apply this new model to 13,245,908 observations of 122,675 SSOs. These observations were acquired in the g and r filters with the Zwicky Transient Facility. We retrieve them and implement the new sHG1G2 model in Fink, a broker of alerts designed for the LSST. The sHG1G2 model leads to smaller residuals than other phase function models, providing a better description of the photometry of asteroids. We determine the absolute magnitude H and phase function coefficients (G1, G2) in each filter, the spin orientation (RA_0,DEC_0), and the polar-to-equatorial oblateness R for 95,593 Solar System Objects (SSOs), which constitutes about a tenfold increase in the number of characterised objects compared to current census. The application of the sHG1G2 model on ZTF alert data using the FINK broker shows that the model is appropriate to extract physical properties of asteroids from multi-band and sparse photometry, such as the forthcoming LSST survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.20179v1-abstract-full').style.display = 'none'; document.getElementById('2403.20179v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A38 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.08548">arXiv:2403.08548</a> <span> [<a href="https://arxiv.org/pdf/2403.08548">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> The Massalia asteroid family as the origin of ordinary L chondrites </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marsset%2C+M">Micha毛l Marsset</a>, <a href="/search/astro-ph?searchtype=author&query=Vernazza%2C+P">Pierre Vernazza</a>, <a href="/search/astro-ph?searchtype=author&query=Bro%C5%BE%2C+M">Miroslav Bro啪</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+C+A">Cristina A. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=DeMeo%2C+F+E">Francesca E. DeMeo</a>, <a href="/search/astro-ph?searchtype=author&query=Burt%2C+B">Brian Burt</a>, <a href="/search/astro-ph?searchtype=author&query=Binzel%2C+R+P">Richard P. Binzel</a>, <a href="/search/astro-ph?searchtype=author&query=Reddy%2C+V">Vishnu Reddy</a>, <a href="/search/astro-ph?searchtype=author&query=McGraw%2C+A">Allison McGraw</a>, <a href="/search/astro-ph?searchtype=author&query=Avdellidou%2C+C">Chrysa Avdellidou</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Slivan%2C+S+M">Stephen M. Slivan</a>, <a href="/search/astro-ph?searchtype=author&query=Polishook%2C+D">David Polishook</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.08548v1-abstract-short" style="display: inline;"> Studies of micrometeorites in mid-Ordovician limestones and Earth's impact craters indicate that our planet witnessed a massive infall of ordinary L chondrite material 466 million years (My) ago (Heck et al. 2017, Schmieder & Kring 2020, Kenkmann 2021) that may have been at the origin of the first major mass extinction event (Schmitz et al. 2019). The breakup of a large asteroid in the main belt i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.08548v1-abstract-full').style.display = 'inline'; document.getElementById('2403.08548v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.08548v1-abstract-full" style="display: none;"> Studies of micrometeorites in mid-Ordovician limestones and Earth's impact craters indicate that our planet witnessed a massive infall of ordinary L chondrite material 466 million years (My) ago (Heck et al. 2017, Schmieder & Kring 2020, Kenkmann 2021) that may have been at the origin of the first major mass extinction event (Schmitz et al. 2019). The breakup of a large asteroid in the main belt is the likely cause of this massive infall. In modern times, material originating from this breakup still dominates meteorite falls (>20% of all falls) (Swindle et al. 2014). Here, we provide spectroscopic observations and dynamical evidence that the Massalia collisional family is the only plausible source of this catastrophic event and of the most abundant class of meteorites falling on Earth today. It is suitably located in the inner belt, at low-inclination orbits, which corresponds to the observed distribution of L-chondrite-like near-Earth objects (NEOs) and of interplanetary dust concentrated at 1.4 degrees (Sykes 1990, Reach et al. 1997). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.08548v1-abstract-full').style.display = 'none'; document.getElementById('2403.08548v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 11 pages, under revision</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.02605">arXiv:2401.02605</a> <span> [<a href="https://arxiv.org/pdf/2401.02605">pdf</a>, <a href="https://arxiv.org/format/2401.02605">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Hubble Asteroid Hunter III. Physical properties of newly found asteroids </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Mart%C3%ADn%2C+P">Pablo Garc铆a-Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S">Sandor Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Popescu%2C+M">Marcel Popescu</a>, <a href="/search/astro-ph?searchtype=author&query=Mer%C3%ADn%2C+B">Bruno Mer铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Stapelfeldt%2C+K+R">Karl R. Stapelfeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+R+W">Robin W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Thomson%2C+R">Ross Thomson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.02605v1-abstract-short" style="display: inline;"> Determining the size distribution of asteroids is key for understanding the collisional history and evolution of the inner Solar System. We aim at improving our knowledge on the size distribution of small asteroids in the Main Belt by determining the parallaxes of newly detected asteroids in the Hubble Space Telescope (HST) Archive and hence their absolute magnitudes and sizes. Asteroids appear as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02605v1-abstract-full').style.display = 'inline'; document.getElementById('2401.02605v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.02605v1-abstract-full" style="display: none;"> Determining the size distribution of asteroids is key for understanding the collisional history and evolution of the inner Solar System. We aim at improving our knowledge on the size distribution of small asteroids in the Main Belt by determining the parallaxes of newly detected asteroids in the Hubble Space Telescope (HST) Archive and hence their absolute magnitudes and sizes. Asteroids appear as curved trails in HST images due to the parallax induced by the fast orbital motion of the spacecraft. The parallax effect can be computed to obtain the distance to the asteroids by fitting simulated trajectories to the observed trails. Using distance, we can obtain the object's absolute magnitude and size estimation assuming an albedo value, along with some boundaries for its orbital parameters. In this work we analyse a set of 632 serendipitously imaged asteroids found in the ESA HST Archive. An object-detection machine learning algorithm was used to perform this task during previous work. Our raw data consists of 1,031 asteroids trails from unknown objects (not matching any entries in the MPC database). We also found 670 trails from known objects (objects featuring matching entries in the MPC). After an accuracy assessment and filtering process, our analysed HST set consists of 454 unknown objects and 178 known objects. We obtain a sample dominated by potential Main Belt objects featuring absolute magnitudes (H) mostly between 15 and 22 mag. The absolute magnitude cumulative distribution confirms the previously reported slope change for 15 < H < 18, from 0.56 to 0.26, maintained in our case down to absolute magnitudes around H = 20, hence expanding the previous results by approximately two magnitudes. HST archival observations can be used as an asteroid survey since the telescope pointings are statistically randomly oriented in the sky and they cover long periods of time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02605v1-abstract-full').style.display = 'none'; document.getElementById('2401.02605v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. 10 pages, 2 tables, 17 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.06551">arXiv:2310.06551</a> <span> [<a href="https://arxiv.org/pdf/2310.06551">pdf</a>, <a href="https://arxiv.org/format/2310.06551">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347203">10.1051/0004-6361/202347203 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Focused Product Release: Sources from Service Interface Function image analysis -- Half a million new sources in omega Centauri </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Weingrill%2C+K">K. Weingrill</a>, <a href="/search/astro-ph?searchtype=author&query=Mints%2C+A">A. Mints</a>, <a href="/search/astro-ph?searchtype=author&query=Casta%C3%B1eda%2C+J">J. Casta帽eda</a>, <a href="/search/astro-ph?searchtype=author&query=Kostrzewa-Rutkowska%2C+Z">Z. Kostrzewa-Rutkowska</a>, <a href="/search/astro-ph?searchtype=author&query=Davidson%2C+M">M. Davidson</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">J. Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Torra%2C+F">F. Torra</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Lerate%2C+M">M. Ramos-Lerate</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Crowley%2C+C">C. Crowley</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn-Fleitas%2C+J+M">J. M. Mart铆n-Fleitas</a>, <a href="/search/astro-ph?searchtype=author&query=Palaversa%2C+L">L. Palaversa</a>, <a href="/search/astro-ph?searchtype=author&query=Mieres%2C+D+R">D. Ruz Mieres</a>, <a href="/search/astro-ph?searchtype=author&query=Tisani%C4%87%2C+K">K. Tisani膰</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Barbier%2C+A">A. Barbier</a> , et al. (378 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.06551v2-abstract-short" style="display: inline;"> Gaia's readout window strategy is challenged by very dense fields in the sky. Therefore, in addition to standard Gaia observations, full Sky Mapper (SM) images were recorded for nine selected regions in the sky. A new software pipeline exploits these Service Interface Function (SIF) images of crowded fields (CFs), making use of the availability of the full two-dimensional (2D) information. This ne… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06551v2-abstract-full').style.display = 'inline'; document.getElementById('2310.06551v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06551v2-abstract-full" style="display: none;"> Gaia's readout window strategy is challenged by very dense fields in the sky. Therefore, in addition to standard Gaia observations, full Sky Mapper (SM) images were recorded for nine selected regions in the sky. A new software pipeline exploits these Service Interface Function (SIF) images of crowded fields (CFs), making use of the availability of the full two-dimensional (2D) information. This new pipeline produced half a million additional Gaia sources in the region of the omega Centauri ($蠅$ Cen) cluster, which are published with this Focused Product Release. We discuss the dedicated SIF CF data reduction pipeline, validate its data products, and introduce their Gaia archive table. Our aim is to improve the completeness of the {\it Gaia} source inventory in a very dense region in the sky, $蠅$ Cen. An adapted version of {\it Gaia}'s Source Detection and Image Parameter Determination software located sources in the 2D SIF CF images. We validated the results by comparing them to the public {\it Gaia} DR3 catalogue and external Hubble Space Telescope data. With this Focused Product Release, 526\,587 new sources have been added to the {\it Gaia} catalogue in $蠅$ Cen. Apart from positions and brightnesses, the additional catalogue contains parallaxes and proper motions, but no meaningful colour information. While SIF CF source parameters generally have a lower precision than nominal {\it Gaia} sources, in the cluster centre they increase the depth of the combined catalogue by three magnitudes and improve the source density by a factor of ten. This first SIF CF data publication already adds great value to the {\it Gaia} catalogue. It demonstrates what to expect for the fourth {\it Gaia} catalogue, which will contain additional sources for all nine SIF CF regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06551v2-abstract-full').style.display = 'none'; document.getElementById('2310.06551v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 680, A35 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.06295">arXiv:2310.06295</a> <span> [<a href="https://arxiv.org/pdf/2310.06295">pdf</a>, <a href="https://arxiv.org/format/2310.06295">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347273">10.1051/0004-6361/202347273 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Focused Product Release: A catalogue of sources around quasars to search for strongly lensed quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Krone-Martins%2C+A">A. Krone-Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Galluccio%2C+L">L. Galluccio</a>, <a href="/search/astro-ph?searchtype=author&query=Delchambre%2C+L">L. Delchambre</a>, <a href="/search/astro-ph?searchtype=author&query=Oreshina-Slezak%2C+I">I. Oreshina-Slezak</a>, <a href="/search/astro-ph?searchtype=author&query=Teixeira%2C+R">R. Teixeira</a>, <a href="/search/astro-ph?searchtype=author&query=Braine%2C+J">J. Braine</a>, <a href="/search/astro-ph?searchtype=author&query=Campion%2C+J+-+L">J. -F. Le Campion</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Roux%2C+W">W. Roux</a>, <a href="/search/astro-ph?searchtype=author&query=Blazere%2C+A">A. Blazere</a>, <a href="/search/astro-ph?searchtype=author&query=Pegoraro%2C+L">L. Pegoraro</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Barbier%2C+A">A. Barbier</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+R">R. Guerra</a> , et al. (376 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.06295v1-abstract-short" style="display: inline;"> Context. Strongly lensed quasars are fundamental sources for cosmology. The Gaia space mission covers the entire sky with the unprecedented resolution of $0.18$" in the optical, making it an ideal instrument to search for gravitational lenses down to the limiting magnitude of 21. Nevertheless, the previous Gaia Data Releases are known to be incomplete for small angular separations such as those ex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06295v1-abstract-full').style.display = 'inline'; document.getElementById('2310.06295v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06295v1-abstract-full" style="display: none;"> Context. Strongly lensed quasars are fundamental sources for cosmology. The Gaia space mission covers the entire sky with the unprecedented resolution of $0.18$" in the optical, making it an ideal instrument to search for gravitational lenses down to the limiting magnitude of 21. Nevertheless, the previous Gaia Data Releases are known to be incomplete for small angular separations such as those expected for most lenses. Aims. We present the Data Processing and Analysis Consortium GravLens pipeline, which was built to analyse all Gaia detections around quasars and to cluster them into sources, thus producing a catalogue of secondary sources around each quasar. We analysed the resulting catalogue to produce scores that indicate source configurations that are compatible with strongly lensed quasars. Methods. GravLens uses the DBSCAN unsupervised clustering algorithm to detect sources around quasars. The resulting catalogue of multiplets is then analysed with several methods to identify potential gravitational lenses. We developed and applied an outlier scoring method, a comparison between the average BP and RP spectra of the components, and we also used an extremely randomised tree algorithm. These methods produce scores to identify the most probable configurations and to establish a list of lens candidates. Results. We analysed the environment of 3 760 032 quasars. A total of 4 760 920 sources, including the quasars, were found within 6" of the quasar positions. This list is given in the Gaia archive. In 87\% of cases, the quasar remains a single source, and in 501 385 cases neighbouring sources were detected. We propose a list of 381 lensed candidates, of which we identified 49 as the most promising. Beyond these candidates, the associate tables in this Focused Product Release allow the entire community to explore the unique Gaia data for strong lensing studies further. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06295v1-abstract-full').style.display = 'none'; document.getElementById('2310.06295v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 60 figures, accepted for publication by Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 685, A130 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.06051">arXiv:2310.06051</a> <span> [<a href="https://arxiv.org/pdf/2310.06051">pdf</a>, <a href="https://arxiv.org/format/2310.06051">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Gaia Focused Product Release: Radial velocity time series of long-period variables </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Trabucchi%2C+M">M. Trabucchi</a>, <a href="/search/astro-ph?searchtype=author&query=Mowlavi%2C+N">N. Mowlavi</a>, <a href="/search/astro-ph?searchtype=author&query=Lebzelter%2C+T">T. Lebzelter</a>, <a href="/search/astro-ph?searchtype=author&query=Lecoeur-Taibi%2C+I">I. Lecoeur-Taibi</a>, <a href="/search/astro-ph?searchtype=author&query=Audard%2C+M">M. Audard</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Lario%2C+P">P. Garc铆a-Lario</a>, <a href="/search/astro-ph?searchtype=author&query=Gavras%2C+P">P. Gavras</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</a>, <a href="/search/astro-ph?searchtype=author&query=de+Fombelle%2C+G+J">G. Jevardat de Fombelle</a>, <a href="/search/astro-ph?searchtype=author&query=Nienartowicz%2C+K">K. Nienartowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Rimoldini%2C+L">L. Rimoldini</a>, <a href="/search/astro-ph?searchtype=author&query=Sartoretti%2C+P">P. Sartoretti</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Fr%C3%A9mat%2C+Y">Y. Fr茅mat</a>, <a href="/search/astro-ph?searchtype=author&query=Marchal%2C+O">O. Marchal</a>, <a href="/search/astro-ph?searchtype=author&query=Damerdji%2C+Y">Y. Damerdji</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Guerrier%2C+A">A. Guerrier</a>, <a href="/search/astro-ph?searchtype=author&query=Panuzzo%2C+P">P. Panuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Katz%2C+D">D. Katz</a>, <a href="/search/astro-ph?searchtype=author&query=Seabroke%2C+G+M">G. M. Seabroke</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+K">K. Benson</a> , et al. (382 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.06051v1-abstract-short" style="display: inline;"> The third Gaia Data Release (DR3) provided photometric time series of more than 2 million long-period variable (LPV) candidates. Anticipating the publication of full radial-velocity (RV) in DR4, this Focused Product Release (FPR) provides RV time series for a selection of LPVs with high-quality observations. We describe the production and content of the Gaia catalog of LPV RV time series, and the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06051v1-abstract-full').style.display = 'inline'; document.getElementById('2310.06051v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06051v1-abstract-full" style="display: none;"> The third Gaia Data Release (DR3) provided photometric time series of more than 2 million long-period variable (LPV) candidates. Anticipating the publication of full radial-velocity (RV) in DR4, this Focused Product Release (FPR) provides RV time series for a selection of LPVs with high-quality observations. We describe the production and content of the Gaia catalog of LPV RV time series, and the methods used to compute variability parameters published in the Gaia FPR. Starting from the DR3 LPVs catalog, we applied filters to construct a sample of sources with high-quality RV measurements. We modeled their RV and photometric time series to derive their periods and amplitudes, and further refined the sample by requiring compatibility between the RV period and at least one of the $G$, $G_{\rm BP}$, or $G_{\rm RP}$ photometric periods. The catalog includes RV time series and variability parameters for 9\,614 sources in the magnitude range $6\lesssim G/{\rm mag}\lesssim 14$, including a flagged top-quality subsample of 6\,093 stars whose RV periods are fully compatible with the values derived from the $G$, $G_{\rm BP}$, and $G_{\rm RP}$ photometric time series. The RV time series contain a mean of 24 measurements per source taken unevenly over a duration of about three years. We identify the great most sources (88%) as genuine LPVs, with about half of them showing a pulsation period and the other half displaying a long secondary period. The remaining 12% consists of candidate ellipsoidal binaries. Quality checks against RVs available in the literature show excellent agreement. We provide illustrative examples and cautionary remarks. The publication of RV time series for almost 10\,000 LPVs constitutes, by far, the largest such database available to date in the literature. The availability of simultaneous photometric measurements gives a unique added value to the Gaia catalog (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06051v1-abstract-full').style.display = 'none'; document.getElementById('2310.06051v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 38 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.03845">arXiv:2310.03845</a> <span> [<a href="https://arxiv.org/pdf/2310.03845">pdf</a>, <a href="https://arxiv.org/format/2310.03845">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347551">10.1051/0004-6361/202347551 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid: Identification of asteroid streaks in simulated images using deep learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=P%C3%B6ntinen%2C+M">M. P枚ntinen</a>, <a href="/search/astro-ph?searchtype=author&query=Granvik%2C+M">M. Granvik</a>, <a href="/search/astro-ph?searchtype=author&query=Nucita%2C+A+A">A. A. Nucita</a>, <a href="/search/astro-ph?searchtype=author&query=Conversi%2C+L">L. Conversi</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Riordan%2C+C+M">C. M. O'Riordan</a>, <a href="/search/astro-ph?searchtype=author&query=Scott%2C+D">D. Scott</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Amendola%2C+L">L. Amendola</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavuoti%2C+S">S. Cavuoti</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cledassou%2C+R">R. Cledassou</a>, <a href="/search/astro-ph?searchtype=author&query=Congedo%2C+G">G. Congedo</a> , et al. (92 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.03845v1-abstract-short" style="display: inline;"> Up to 150000 asteroids will be visible in the images of the ESA Euclid space telescope, and the instruments of Euclid offer multiband visual to near-infrared photometry and slitless spectra of these objects. Most asteroids will appear as streaks in the images. Due to the large number of images and asteroids, automated detection methods are needed. A non-machine-learning approach based on the Strea… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.03845v1-abstract-full').style.display = 'inline'; document.getElementById('2310.03845v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.03845v1-abstract-full" style="display: none;"> Up to 150000 asteroids will be visible in the images of the ESA Euclid space telescope, and the instruments of Euclid offer multiband visual to near-infrared photometry and slitless spectra of these objects. Most asteroids will appear as streaks in the images. Due to the large number of images and asteroids, automated detection methods are needed. A non-machine-learning approach based on the StreakDet software was previously tested, but the results were not optimal for short and/or faint streaks. We set out to improve the capability to detect asteroid streaks in Euclid images by using deep learning. We built, trained, and tested a three-step machine-learning pipeline with simulated Euclid images. First, a convolutional neural network (CNN) detected streaks and their coordinates in full images, aiming to maximize the completeness (recall) of detections. Then, a recurrent neural network (RNN) merged snippets of long streaks detected in several parts by the CNN. Lastly, gradient-boosted trees (XGBoost) linked detected streaks between different Euclid exposures to reduce the number of false positives and improve the purity (precision) of the sample. The deep-learning pipeline surpasses the completeness and reaches a similar level of purity of a non-machine-learning pipeline based on the StreakDet software. Additionally, the deep-learning pipeline can detect asteroids 0.25-0.5 magnitudes fainter than StreakDet. The deep-learning pipeline could result in a 50% increase in the number of detected asteroids compared to the StreakDet software. There is still scope for further refinement, particularly in improving the accuracy of streak coordinates and enhancing the completeness of the final stage of the pipeline, which involves linking detections across multiple exposures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.03845v1-abstract-full').style.display = 'none'; document.getElementById('2310.03845v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 679, A135 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.15537">arXiv:2309.15537</a> <span> [<a href="https://arxiv.org/pdf/2309.15537">pdf</a>, <a href="https://arxiv.org/format/2309.15537">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347158">10.1051/0004-6361/202347158 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Close-to-fission dumbbell Jupiter-Trojan (17365) Thymbraeus </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Descamps%2C+P">P. Descamps</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrais%2C+M">M. Ferrais</a>, <a href="/search/astro-ph?searchtype=author&query=Rivet%2C+J+-">J. -P. Rivet</a>, <a href="/search/astro-ph?searchtype=author&query=Berthier%2C+J">J. Berthier</a>, <a href="/search/astro-ph?searchtype=author&query=Jehin%2C+E">E. Jehin</a>, <a href="/search/astro-ph?searchtype=author&query=Vernet%2C+D">D. Vernet</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+L">L. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Bendjoya%2C+P">P. Bendjoya</a>, <a href="/search/astro-ph?searchtype=author&query=Vachier%2C+F">F. Vachier</a>, <a href="/search/astro-ph?searchtype=author&query=Pajuelo%2C+M">M. Pajuelo</a>, <a href="/search/astro-ph?searchtype=author&query=Birlan%2C+M">M. Birlan</a>, <a href="/search/astro-ph?searchtype=author&query=Colas%2C+F">F. Colas</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhaldoun%2C+Z">Z. Benkhaldoun</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.15537v1-abstract-short" style="display: inline;"> Every population of small bodies in the Solar system contains a sizable fraction of multiple systems. Among these, the Jupiter Trojans have the lowest number of known binary systems and the least characterized. We aim at characterizing the reported binary system (17365) Thymbraeus, one of the only seven multiple systems known among Jupiter Trojans. We conducted light curves observing campaigns in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.15537v1-abstract-full').style.display = 'inline'; document.getElementById('2309.15537v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.15537v1-abstract-full" style="display: none;"> Every population of small bodies in the Solar system contains a sizable fraction of multiple systems. Among these, the Jupiter Trojans have the lowest number of known binary systems and the least characterized. We aim at characterizing the reported binary system (17365) Thymbraeus, one of the only seven multiple systems known among Jupiter Trojans. We conducted light curves observing campaigns in 2013, 2015, and 2021 with ground-based telescopes. We model these lightcurves using dumbbell equilibrium figures. We show that Thymbraeus is unlikely a binary system. Its light curves are fully consistent with a bilobated shape: a dumbbell equilibrium figure. We determine a low density of 830 +/- 50 kg.m-3 , consistent with the reported density of other Jupiter Trojan asteroids and small Kuiper-belt objects. The angular velocity of Thymbraeus is close to fission. If separated, its components would become a similarly-sized double asteroid such as the other Jupiter Trojan (617) Patroclus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.15537v1-abstract-full').style.display = 'none'; document.getElementById('2309.15537v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 680, A21 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.03555">arXiv:2309.03555</a> <span> [<a href="https://arxiv.org/pdf/2309.03555">pdf</a>, <a href="https://arxiv.org/format/2309.03555">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346394">10.1051/0004-6361/202346394 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Compositional properties of planet-crossing asteroids from astronomical surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sergeyev%2C+A+V">A. V. Sergeyev</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Marsset%2C+M">M. Marsset</a>, <a href="/search/astro-ph?searchtype=author&query=Pravec%2C+P">P. Pravec</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+D">D. Perna</a>, <a href="/search/astro-ph?searchtype=author&query=DeMeo%2C+F+E">F. E. DeMeo</a>, <a href="/search/astro-ph?searchtype=author&query=Petropoulou%2C+V">V. Petropoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Lazzarin%2C+M">M. Lazzarin</a>, <a href="/search/astro-ph?searchtype=author&query=La+Forgia%2C+F">F. La Forgia</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Petro%2C+I">I. Di Petro</a>, <a href="/search/astro-ph?searchtype=author&query=team%2C+t+N">the NEOROCKS team</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.03555v1-abstract-short" style="display: inline;"> Context. The study of planet-crossing asteroids is of both practical and fundamental importance. As they are closer than asteroids in the Main Belt, we have access to a smaller size range, and this population frequently impacts planetary surfaces and can pose a threat to life. Aims. We aim to characterize the compositions of a large corpus of planet-crossing asteroids and to study how these compos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03555v1-abstract-full').style.display = 'inline'; document.getElementById('2309.03555v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03555v1-abstract-full" style="display: none;"> Context. The study of planet-crossing asteroids is of both practical and fundamental importance. As they are closer than asteroids in the Main Belt, we have access to a smaller size range, and this population frequently impacts planetary surfaces and can pose a threat to life. Aims. We aim to characterize the compositions of a large corpus of planet-crossing asteroids and to study how these compositions are related to orbital and physical parameters. Methods. We gathered publicly available visible colors of near-Earth objects (NEOs) from the Sloan Digital Sky Survey (SDSS) and SkyMapper surveys. We also computed SDSS-compatible colors from reflectance spectra of the Gaia mission and a compilation of ground-based observations. We determined the taxonomy of each NEO from its colors and studied the distribution of the taxonomic classes and spectral slope against the orbital parameters and diameter. Results. We provide updated photometry for 470 NEOs from the SDSS, and taxonomic classification of 7,401 NEOs. We classify 42 NEOs that are mission-accessible, including six of the seven flyby candidates of the ESA Hera mission. We confirm the perihelion dependance of spectral slope among S-type NEOs, likely related to a rejuvenation mechanism linked with thermal fatigue. We also confirm the clustering of A-type NEOs around 1.5-2 AU, and predict the taxonomic distribution of small asteroids in the NEO source regions in the Main Belt. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03555v1-abstract-full').style.display = 'none'; document.getElementById('2309.03555v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 27 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 679, A148 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.10056">arXiv:2307.10056</a> <span> [<a href="https://arxiv.org/pdf/2307.10056">pdf</a>, <a href="https://arxiv.org/format/2307.10056">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad2150">10.1093/mnras/stad2150 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Speckle observations of the binary asteroid (22) Kalliope with C2PU/PISCO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aristidi%2C+E">E. Aristidi</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Minker%2C+K">K. Minker</a>, <a href="/search/astro-ph?searchtype=author&query=Prieur%2C+J+-">J. -L. Prieur</a>, <a href="/search/astro-ph?searchtype=author&query=Scardia%2C+M">M. Scardia</a>, <a href="/search/astro-ph?searchtype=author&query=Rivet%2C+J+-">J. -P. Rivet</a>, <a href="/search/astro-ph?searchtype=author&query=Bendjoya%2C+P">P. Bendjoya</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+L">L. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Argyle%2C+R+-">R. -W. Argyle</a>, <a href="/search/astro-ph?searchtype=author&query=Koechlin%2C+L">L. Koechlin</a>, <a href="/search/astro-ph?searchtype=author&query=Ling%2C+J+F">J. F. Ling</a>, <a href="/search/astro-ph?searchtype=author&query=Maccarini%2C+L">L. Maccarini</a>, <a href="/search/astro-ph?searchtype=author&query=Pansecchi%2C+L">L. Pansecchi</a>, <a href="/search/astro-ph?searchtype=author&query=Piccotti%2C+L">L. Piccotti</a>, <a href="/search/astro-ph?searchtype=author&query=Serot%2C+J">J. Serot</a>, <a href="/search/astro-ph?searchtype=author&query=Vernet%2C+D">D. Vernet</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.10056v1-abstract-short" style="display: inline;"> We present new speckle measurements of the position of Linus, the satellite of the asteroid (22) Kalliope, obtained at the 1m C2PU-Epsilon telescope on the Plateau de Calern, France. Observations were made in the visible domain with the speckle camera PISCO. We obtained 122 measurements in February-March 2022 and April 2023, with a mean uncertainty close to 10 milli-arcseconds on the angular separ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10056v1-abstract-full').style.display = 'inline'; document.getElementById('2307.10056v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.10056v1-abstract-full" style="display: none;"> We present new speckle measurements of the position of Linus, the satellite of the asteroid (22) Kalliope, obtained at the 1m C2PU-Epsilon telescope on the Plateau de Calern, France. Observations were made in the visible domain with the speckle camera PISCO. We obtained 122 measurements in February-March 2022 and April 2023, with a mean uncertainty close to 10 milli-arcseconds on the angular separation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10056v1-abstract-full').style.display = 'none'; document.getElementById('2307.10056v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.04768">arXiv:2306.04768</a> <span> [<a href="https://arxiv.org/pdf/2306.04768">pdf</a>, <a href="https://arxiv.org/format/2306.04768">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346326">10.1051/0004-6361/202346326 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 2021 occultations and transits of Linus orbiting (22) Kalliope: I. Polygonal and `cliptracing' algorithm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bro%C5%BE%2C+M">M. Bro啪</a>, <a href="/search/astro-ph?searchtype=author&query=%C4%8Eurech%2C+J">J. 膸urech</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrais%2C+M">M. Ferrais</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+H+-">H. -J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+M+-">M. -J. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Roh%2C+D+-">D. -G. Roh</a>, <a href="/search/astro-ph?searchtype=author&query=Yim%2C+H+-">H. -S. Yim</a>, <a href="/search/astro-ph?searchtype=author&query=Jehin%2C+E">E. Jehin</a>, <a href="/search/astro-ph?searchtype=author&query=Burdanov%2C+A">A. Burdanov</a>, <a href="/search/astro-ph?searchtype=author&query=de+Wit%2C+J">J. de Wit</a>, <a href="/search/astro-ph?searchtype=author&query=Fatka%2C+P">P. Fatka</a>, <a href="/search/astro-ph?searchtype=author&query=Hanu%C5%A1%2C+J">J. Hanu拧</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.04768v1-abstract-short" style="display: inline;"> The satellite Linus orbiting the main-belt asteroid (22) Kalliope exhibited occultation and transit events in late 2021. A photometric campaign was organized and observations were taken by the TRAPPIST-South, SPECULOOS-Artemis, OWL-Net, and BOAO telescopes, with the goal to constrain models of this system. Our dynamical model is complex, with multipoles (up to the order $\ell = 2$), internal tides… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04768v1-abstract-full').style.display = 'inline'; document.getElementById('2306.04768v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.04768v1-abstract-full" style="display: none;"> The satellite Linus orbiting the main-belt asteroid (22) Kalliope exhibited occultation and transit events in late 2021. A photometric campaign was organized and observations were taken by the TRAPPIST-South, SPECULOOS-Artemis, OWL-Net, and BOAO telescopes, with the goal to constrain models of this system. Our dynamical model is complex, with multipoles (up to the order $\ell = 2$), internal tides, and external tides. The model was constrained by astrometry (spanning 2001--2021), occultations, adaptive-optics imaging, calibrated photometry, as well as relative photometry. Our photometric model was substantially improved. A new precise (${<}\,0.1\,{\rm mmag}$) light curve algorithm was implemented, based on polygon intersections, which are computed exactly -- by including partial eclipses and partial visibility of polygons. Moreover, we implemented a `cliptracing' algorithm, based again on polygon intersections, in which partial contributions to individual pixels are computed exactly. Both synthetic light curves and synthetic images are then very smooth. Based on our combined solution, we confirmed the size of Linus, $(28\pm 1)\,{\rm km}$. However, this solution exhibits some tension between the light curves and the PISCO speckle-interferometry dataset. In most solutions, Linus is darker than Kalliope, with the albedos $A_{\rm w} = 0.40$ vs. $0.44$. This is confirmed on deconvolved images. A~detailed revision of astrometric data allowed us to revise also the $J_2 \equiv -C_{20}$ value of Kalliope. Most importantly, a~homogeneous body is excluded. For a differentiated body, two solutions exist: low-oblateness ($C_{20} \simeq -0.12$), with a~spherical iron core, and alternatively, high-oblateness ($C_{20} \simeq -0.22$) with an elongated iron core. These correspond to the low- and high-energy collisions, respectively, studied by means of SPH simulations in our previous work. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04768v1-abstract-full').style.display = 'none'; document.getElementById('2306.04768v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astronomy and Astrophysics, accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, A60 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.01834">arXiv:2306.01834</a> <span> [<a href="https://arxiv.org/pdf/2306.01834">pdf</a>, <a href="https://arxiv.org/format/2306.01834">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346032">10.1051/0004-6361/202346032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectral analogues of Barbarian asteroids among CO and CV chondrites </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mahlke%2C+M">Max Mahlke</a>, <a href="/search/astro-ph?searchtype=author&query=Eschrig%2C+J">Jolantha Eschrig</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Bonal%2C+L">Lydie Bonal</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+P">Pierre Beck</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.01834v1-abstract-short" style="display: inline;"> K- and L-type asteroids are considered to be the parent bodies of CV and CO chondrites. Spectral models of L-types invoke an enrichment in CAI with respect to the chondrites in the meteorite collection. Barbarian asteroids are associated to L-type asteroids yet the relationship between these populations is still not clear. We aim to investigate the link between the K- and L-type and Barbarian aste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.01834v1-abstract-full').style.display = 'inline'; document.getElementById('2306.01834v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.01834v1-abstract-full" style="display: none;"> K- and L-type asteroids are considered to be the parent bodies of CV and CO chondrites. Spectral models of L-types invoke an enrichment in CAI with respect to the chondrites in the meteorite collection. Barbarian asteroids are associated to L-type asteroids yet the relationship between these populations is still not clear. We aim to investigate the link between the K- and L-type and Barbarian asteroids and the CV and CO chondrites by means of spectral matching of a large number of reflectance spectra of objects from either population. We seek to identify matches based on observed rather than modelled spectral features. We employ a matching criterion that accounts for the residuals and the correlation of the spectral features. The only free parameter in the comparison is the degree of alteration of the asteroids with respect to the meteorites expressed via an exponential model. We derive an absolute scale of similarity between the spectra using laboratory data from irradiation experiments. CVOxA chondrites are the best match to the asteroids, in particular to K-type (7 out of 11 asteroids matched) and Barbarians (11 out of 16). CO chondrites provide convincing matches for K-types (5 out of 11) and Barbarians (7 out of 16) as well. A single non-Barbarian L-type is matched to a meteorite. Only a few asteroids are matched to CVOxB and CVRed chondrites. Barbarian asteroids are represented among CO and CVOxA chondrites without requiring an enrichment of CAI in the asteroids. Four candidate Barbarian asteroids are identified, three of which are classified as K-types. These asteroids are favourable targets for polarimetric observations. The discrepancy between L-type asteroids and CV and CO chondrites is likely related to the ambiguity of the asteroid class itself. An extension of the taxonomy to include polarimetric properties is required. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.01834v1-abstract-full').style.display = 'none'; document.getElementById('2306.01834v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, A94 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.01123">arXiv:2305.01123</a> <span> [<a href="https://arxiv.org/pdf/2305.01123">pdf</a>, <a href="https://arxiv.org/format/2305.01123">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346905">10.1051/0004-6361/202346905 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Enabling discovery of solar system objects in large alert data streams </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Montagner%2C+R+L">R. Le Montagner</a>, <a href="/search/astro-ph?searchtype=author&query=Peloton%2C+J">J. Peloton</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Desmars%2C+J">J. Desmars</a>, <a href="/search/astro-ph?searchtype=author&query=Hestroffer%2C+D">D. Hestroffer</a>, <a href="/search/astro-ph?searchtype=author&query=Mendez%2C+R+A">R. A. Mendez</a>, <a href="/search/astro-ph?searchtype=author&query=Perlbarg%2C+A+C">A. C. Perlbarg</a>, <a href="/search/astro-ph?searchtype=author&query=Thuillot%2C+W">W. Thuillot</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.01123v2-abstract-short" style="display: inline;"> With the advent of large-scale astronomical surveys such as the Zwicky Transient Facility (ZTF), the number of alerts generated by transient, variable and moving astronomical objects is growing rapidly, reaching millions per night. Concerning solar system minor planets, their identification requires linking the alerts of many observations over a potentially large time, leading to a very large comb… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.01123v2-abstract-full').style.display = 'inline'; document.getElementById('2305.01123v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.01123v2-abstract-full" style="display: none;"> With the advent of large-scale astronomical surveys such as the Zwicky Transient Facility (ZTF), the number of alerts generated by transient, variable and moving astronomical objects is growing rapidly, reaching millions per night. Concerning solar system minor planets, their identification requires linking the alerts of many observations over a potentially large time, leading to a very large combinatorial number. This work aims to identify new candidates for solar system objects from massive alert data streams produced by large-scale surveys, such as the ZTF and the Vera C. Rubin Observatory's Legacy Survey of Space and Time. Our analysis used the Fink alert broker capabilities to reduce the 111,275,131 processed alerts from ZTF between November 2019 and December 2022 to only 389,530 new solar system alert candidates over the same period. We then implemented a linking algorithm, Fink-FAT, to create real-time trajectory candidates from alert data and extract orbital parameters. The analysis was validated on ZTF alert packets linked to confirmed solar system objects from the Minor Planet Center database. Finally, the results were confronted against follow-up observations. Between November 2019 and December 2022, Fink-FAT extracted 327 new orbits from solar system object candidates at the time of the observations, over which 65 were still unreported in the MPC database as of March 2023. After two late follow-up observation campaigns of six orbit candidates, four were associated with known solar system minor planets, and two remain unknown. Fink-FAT is deployed in the Fink broker and successfully analyzes in real time the alert data from the ZTF survey by regularly extracting new candidates for solar system objects. Our scalability tests also show that Fink-FAT can handle the even larger volume of alert data that the Rubin Observatory will send. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.01123v2-abstract-full').style.display = 'none'; document.getElementById('2305.01123v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.02668">arXiv:2302.02668</a> <span> [<a href="https://arxiv.org/pdf/2302.02668">pdf</a>, <a href="https://arxiv.org/ps/2302.02668">ps</a>, <a href="https://arxiv.org/format/2302.02668">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245538">10.1051/0004-6361/202245538 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deficit of primitive compositions in binary asteroids and pairs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Minker%2C+K">Kate Minker</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Beno卯t Carry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.02668v1-abstract-short" style="display: inline;"> Context. Small binary asteroid systems and pairs are thought to form through fission induced by spin up via the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect. This process is expected to depend on their structural strength, hence composition. Aims. We aim to determine how taxonomic classes, used as a proxy for composition, distribute amongst binary asteroids and asteroid pairs compared to th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02668v1-abstract-full').style.display = 'inline'; document.getElementById('2302.02668v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.02668v1-abstract-full" style="display: none;"> Context. Small binary asteroid systems and pairs are thought to form through fission induced by spin up via the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect. This process is expected to depend on their structural strength, hence composition. Aims. We aim to determine how taxonomic classes, used as a proxy for composition, distribute amongst binary asteroids and asteroid pairs compared to the general population. Methods. We compare the distribution of taxonomic classes of binary systems and pairs with that of a reference sample of asteroids. We build this sample by selecting asteroids to reproduce the orbital and size distribution of the binaries and pairs to minimize potential biases between samples. Results. A strong deficit of primitive compositions (C, B, P, D types) among binary asteroids and asteroid pairs is identified, as well as a strong excess of asteroids with mafic-silicate rich surface compositions (S, Q, V, A types). Conclusions. Amongst low mass, rapidly rotating asteroids, those with mafic-silicate rich compositions are more likely to form multiple asteroid systems than their primitive counterparts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02668v1-abstract-full').style.display = 'none'; document.getElementById('2302.02668v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 7 figures, last 5 pages are tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A48 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.00680">arXiv:2212.00680</a> <span> [<a href="https://arxiv.org/pdf/2212.00680">pdf</a>, <a href="https://arxiv.org/format/2212.00680">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243859">10.1051/0004-6361/202243859 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The equilibrium shape of (65) Cybele: primordial or relic of a large impact? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marsset%2C+M">M. Marsset</a>, <a href="/search/astro-ph?searchtype=author&query=Bro%C5%BE%2C+M">M. Bro啪</a>, <a href="/search/astro-ph?searchtype=author&query=Vermersch%2C+J">J. Vermersch</a>, <a href="/search/astro-ph?searchtype=author&query=Rambaux%2C+N">N. Rambaux</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrais%2C+M">M. Ferrais</a>, <a href="/search/astro-ph?searchtype=author&query=Viikinkoski%2C+M">M. Viikinkoski</a>, <a href="/search/astro-ph?searchtype=author&query=Hanu%C5%A1%2C+J">J. Hanu拧</a>, <a href="/search/astro-ph?searchtype=author&query=Jehin%2C+E">E. Jehin</a>, <a href="/search/astro-ph?searchtype=author&query=Podlewska-Gaca%2C+E">E. Podlewska-Gaca</a>, <a href="/search/astro-ph?searchtype=author&query=Bartczak%2C+P">P. Bartczak</a>, <a href="/search/astro-ph?searchtype=author&query=Dudzinski%2C+G">G. Dudzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Vernazza%2C+P">P. Vernazza</a>, <a href="/search/astro-ph?searchtype=author&query=Szak%C3%A1ts%2C+R">R. Szak谩ts</a>, <a href="/search/astro-ph?searchtype=author&query=Duffard%2C+R">R. Duffard</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+A">A. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Molina%2C+D">D. Molina</a>, <a href="/search/astro-ph?searchtype=author&query=Santana-Ros%2C+T">T. Santana-Ros</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhaldoun%2C+Z">Z. Benkhaldoun</a>, <a href="/search/astro-ph?searchtype=author&query=Birlan%2C+M">M. Birlan</a>, <a href="/search/astro-ph?searchtype=author&query=Dumas%2C+C">C. Dumas</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%A9tick%2C+R">R. F茅tick</a>, <a href="/search/astro-ph?searchtype=author&query=Fusco%2C+T">T. Fusco</a>, <a href="/search/astro-ph?searchtype=author&query=Jorda%2C+L">L. Jorda</a>, <a href="/search/astro-ph?searchtype=author&query=Marchis%2C+F">F. Marchis</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.00680v1-abstract-short" style="display: inline;"> Cybele asteroids constitute an appealing reservoir of primitive material genetically linked to the outer Solar System, and the physical properties of the largest members can be readily accessed by large telescopes. We took advantage of the bright apparition of (65) Cybele in July and August 2021 to acquire high-angular-resolution images and optical light curves of the asteroid with which we aim to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00680v1-abstract-full').style.display = 'inline'; document.getElementById('2212.00680v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.00680v1-abstract-full" style="display: none;"> Cybele asteroids constitute an appealing reservoir of primitive material genetically linked to the outer Solar System, and the physical properties of the largest members can be readily accessed by large telescopes. We took advantage of the bright apparition of (65) Cybele in July and August 2021 to acquire high-angular-resolution images and optical light curves of the asteroid with which we aim to analyse its shape and bulk properties. 7 series of images acquired with VLT/SPHERE were combined with optical light curves to reconstruct the shape of the asteroid using the ADAM, MPCD, and SAGE algorithms. The origin of the shape was investigated by means of N-body simulations. Cybele has a volume-equivalent diameter of 263+/-3km and a bulk density of 1.55+/-0.19g.cm-3. Notably, its shape and rotation state are closely compatible with those of a Maclaurin equilibrium figure. The lack of a collisional family associated with Cybele and the higher bulk density of that body with respect to other large P-type asteroids suggest that it never experienced any large disruptive impact followed by rapid re-accumulation. This would imply that its present-day shape represents the original one. However, numerical integration of the long-term dynamical evolution of a hypothetical family shows that it is dispersed by gravitational perturbations and chaotic diffusion over Gyrs of evolution. The very close match between Cybele and an equilibrium figure opens up the possibility that D>260km small bodies from the outer Solar System all formed at equilibrium. However, we cannot rule out an old impact as the origin of the equilibrium shape. Cybele itself is found to be dynamically unstable, implying that it was recently (<1Ga) placed on its current orbit either through slow diffusion from a relatively stable orbit in the Cybele region or, less likely, from an unstable, JFC orbit in the planet-crossing region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00680v1-abstract-full').style.display = 'none'; document.getElementById('2212.00680v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 14 figures, 4 tables, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.12313">arXiv:2211.12313</a> <span> [<a href="https://arxiv.org/pdf/2211.12313">pdf</a>, <a href="https://arxiv.org/ps/2211.12313">ps</a>, <a href="https://arxiv.org/format/2211.12313">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac3442">10.1093/mnras/stac3442 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectral analysis of basaltic asteroids observed by the Gaia space mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oszkiewicz%2C+D">Dagmara Oszkiewicz</a>, <a href="/search/astro-ph?searchtype=author&query=Klimczak%2C+H">Hanna Klimczak</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Penttila%2C+A">Antti Penttila</a>, <a href="/search/astro-ph?searchtype=author&query=Popescu%2C+M">Marcel Popescu</a>, <a href="/search/astro-ph?searchtype=author&query=Kruger%2C+J">Joahim Kruger</a>, <a href="/search/astro-ph?searchtype=author&query=Keniger%2C+M+A">Marcelo Aron Keniger</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.12313v1-abstract-short" style="display: inline;"> There is a great deal of scientific interest in characterizing the basaltic asteroids (spectrally classified as V-types), as they are the key to understanding planetesimal formation and evolution in the early Solar System. These have long been recognized as parts of the crusts of fully differentiated planetesimals. Thus, their multiplicity, distribution, and physical characteristics are crucial fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.12313v1-abstract-full').style.display = 'inline'; document.getElementById('2211.12313v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.12313v1-abstract-full" style="display: none;"> There is a great deal of scientific interest in characterizing the basaltic asteroids (spectrally classified as V-types), as they are the key to understanding planetesimal formation and evolution in the early Solar System. These have long been recognized as parts of the crusts of fully differentiated planetesimals. Thus, their multiplicity, distribution, and physical characteristics are crucial for providing context for and constraining the theoretical evolution models of the Solar System. In this work, we perform spectral analysis with an extended data set of spectral measurements from the ESA Gaia mission Data Release 3, thus increasing the sample size of the analyzed V-types by more than three times as compared to the literature. Using the data provided by Gaia we identified ~2000 possible V-type asteroids. About 350 of them successfully pass our data validation criteria. This sample includes 31 new V-type asteroids beyond 2.5 au and 6 in the Phocaea region. We confirm that the V-type asteroids in the middle and outer part of the main belt show distinct spectral properties compared to typical vestoids. In the inner main belt, we found a great diversity of spectral parameters among the V-types in all populations. Number of asteroids show band depths even greater than that of (1459) Magnya. Furthermore, some objects present 0.9~\textmu{}m band-centers more than one standard deviation away from the typical value for vestoids. However since the DR3 band centers are often overestimated, those findings are to be confirmed. Overall our results indicate that the inner main belt may contain remnants of multiple differentiated planetesimals, not just (4) Vesta. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.12313v1-abstract-full').style.display = 'none'; document.getElementById('2211.12313v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.10697">arXiv:2209.10697</a> <span> [<a href="https://arxiv.org/pdf/2209.10697">pdf</a>, <a href="https://arxiv.org/format/2209.10697">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244878">10.1051/0004-6361/202244878 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SsODNet: The Solar system Open Database Network </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Berthier%2C+J">J. Berthier</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Mahlke%2C+M">M. Mahlke</a>, <a href="/search/astro-ph?searchtype=author&query=Normand%2C+J">J. Normand</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.10697v4-abstract-short" style="display: inline;"> The sample of Solar system objects has dramatically increased over the last decade. The amount of measured properties (e.g., diameter, taxonomy, rotation period, thermal inertia) has grown even faster. However, this wealth of information is spread over a myriad of articles, under many different designations per object. We provide a solution to the identification of Solar system objects from any of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.10697v4-abstract-full').style.display = 'inline'; document.getElementById('2209.10697v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.10697v4-abstract-full" style="display: none;"> The sample of Solar system objects has dramatically increased over the last decade. The amount of measured properties (e.g., diameter, taxonomy, rotation period, thermal inertia) has grown even faster. However, this wealth of information is spread over a myriad of articles, under many different designations per object. We provide a solution to the identification of Solar system objects from any of their multiple names or designations. We also compile and rationalize their properties to provide an easy access to them. We aim to continuously update the database as new measurements become available. We built a Web Service, SsODNet, that offers four access points, each corresponding to an identified necessity in the community: name resolution (quaero), compilation of a large corpus of properties (datacloud), determination of the best estimate among compiled values (ssoCard), and statistical description of the population (ssoBFT). The SsODNet interfaces are fully operational and freely accessible to everyone. The name resolver quaero translates any of the ~5.3 million designations of objects into their current official designation. The datacloud compiles about 105 million parameters (osculating and proper elements, pair and family membership, diameter, albedo, mass, density, rotation period, spin coordinates, phase function parameters, colors, taxonomy, thermal inertia, and Yarkovsky drift) from over 3,000 articles (and growing). For each of the known asteroids and dwarf planets (~1.2 million), a ssoCard providing a single best-estimate for each parameter is available. The SsODNet service provides these resources in a fraction of second upon query. Finally, the large ssoBFT table compiles all the best-estimates in a single table for population-wide studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.10697v4-abstract-full').style.display = 'none'; document.getElementById('2209.10697v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, A151 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.02092">arXiv:2209.02092</a> <span> [<a href="https://arxiv.org/pdf/2209.02092">pdf</a>, <a href="https://arxiv.org/format/2209.02092">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Upgrading the high contrast imaging facility SPHERE: science drivers and instrument choices </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Chauvin%2C+G">G. Chauvin</a>, <a href="/search/astro-ph?searchtype=author&query=Wildi%2C+F">F. Wildi</a>, <a href="/search/astro-ph?searchtype=author&query=Milli%2C+J">J. Milli</a>, <a href="/search/astro-ph?searchtype=author&query=Stadler%2C+E">E. Stadler</a>, <a href="/search/astro-ph?searchtype=author&query=Diolaiti%2C+E">E. Diolaiti</a>, <a href="/search/astro-ph?searchtype=author&query=Gratton%2C+R">R. Gratton</a>, <a href="/search/astro-ph?searchtype=author&query=Vidal%2C+F">F. Vidal</a>, <a href="/search/astro-ph?searchtype=author&query=Loupias%2C+M">M. Loupias</a>, <a href="/search/astro-ph?searchtype=author&query=Langlois%2C+M">M. Langlois</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">F. Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=N%27Diaye%2C+M">M. N'Diaye</a>, <a href="/search/astro-ph?searchtype=author&query=Gratadour%2C+D">D. Gratadour</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+F">F. Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Tallon%2C+M">M. Tallon</a>, <a href="/search/astro-ph?searchtype=author&query=Mazoyer%2C+J">J. Mazoyer</a>, <a href="/search/astro-ph?searchtype=author&query=Segransan%2C+D">D. Segransan</a>, <a href="/search/astro-ph?searchtype=author&query=Mouillet%2C+D">D. Mouillet</a>, <a href="/search/astro-ph?searchtype=author&query=Beuzit%2C+J+-">J. -L. Beuzit</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Galicher%2C+R">R. Galicher</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I">I. Snellen</a>, <a href="/search/astro-ph?searchtype=author&query=Feldt%2C+M">M. Feldt</a>, <a href="/search/astro-ph?searchtype=author&query=Desidera%2C+S">S. Desidera</a> , et al. (49 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.02092v1-abstract-short" style="display: inline;"> SPHERE+ is a proposed upgrade of the SPHERE instrument at the VLT, which is intended to boost the current performances of detection and characterization for exoplanets and disks. SPHERE+ will also serve as a demonstrator for the future planet finder (PCS) of the European ELT. The main science drivers for SPHERE+ are 1/ to access the bulk of the young giant planet population down to the snow line (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.02092v1-abstract-full').style.display = 'inline'; document.getElementById('2209.02092v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.02092v1-abstract-full" style="display: none;"> SPHERE+ is a proposed upgrade of the SPHERE instrument at the VLT, which is intended to boost the current performances of detection and characterization for exoplanets and disks. SPHERE+ will also serve as a demonstrator for the future planet finder (PCS) of the European ELT. The main science drivers for SPHERE+ are 1/ to access the bulk of the young giant planet population down to the snow line ($3-10$ au), to bridge the gap with complementary techniques (radial velocity, astrometry); 2/ to observe fainter and redder targets in the youngest ($1-10$\,Myr) associations compared to those observed with SPHERE to directly study the formation of giant planets in their birth environment; 3/ to improve the level of characterization of exoplanetary atmospheres by increasing the spectral resolution in order to break degeneracies in giant planet atmosphere models. Achieving these objectives requires to increase the bandwidth of the xAO system (from $\sim$1 to 3\,kHz) as well as the sensitivity in the infrared (2 to 3\,mag). These features will be brought by a second stage AO system optimized in the infrared with a pyramid wavefront sensor. As a new science instrument, a medium resolution integral field spectrograph will provide a spectral resolution from 1000 to 5000 in the J and H bands. This paper gives an overview of the science drivers, requirements and key instrumental trade-off that were done for SPHERE+ to reach the final selected baseline concept. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.02092v1-abstract-full').style.display = 'none'; document.getElementById('2209.02092v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in the Proceedings of the SPIE Astronomical Telescopes + Instrumentation (2022), 13 pages, 6 figure</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.00211">arXiv:2208.00211</a> <span> [<a href="https://arxiv.org/pdf/2208.00211">pdf</a>, <a href="https://arxiv.org/format/2208.00211">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243940">10.1051/0004-6361/202243940 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Summary of the content and survey properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+R">R. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U+L">U. L. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Luri%2C+X">X. Luri</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Panem%2C+C">C. Panem</a>, <a href="/search/astro-ph?searchtype=author&query=Pourbaix%2C+D">D. Pourbaix</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Sartoretti%2C+P">P. Sartoretti</a>, <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</a> , et al. (431 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.00211v1-abstract-short" style="display: inline;"> We present the third data release of the European Space Agency's Gaia mission, GDR3. The GDR3 catalogue is the outcome of the processing of raw data collected with the Gaia instruments during the first 34 months of the mission by the Gaia Data Processing and Analysis Consortium. The GDR3 catalogue contains the same source list, celestial positions, proper motions, parallaxes, and broad band photom… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00211v1-abstract-full').style.display = 'inline'; document.getElementById('2208.00211v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.00211v1-abstract-full" style="display: none;"> We present the third data release of the European Space Agency's Gaia mission, GDR3. The GDR3 catalogue is the outcome of the processing of raw data collected with the Gaia instruments during the first 34 months of the mission by the Gaia Data Processing and Analysis Consortium. The GDR3 catalogue contains the same source list, celestial positions, proper motions, parallaxes, and broad band photometry in the G, G$_{BP}$, and G$_{RP}$ pass-bands already present in the Early Third Data Release. GDR3 introduces an impressive wealth of new data products. More than 33 million objects in the ranges $G_{rvs} < 14$ and $3100 <T_{eff} <14500 $, have new determinations of their mean radial velocities based on data collected by Gaia. We provide G$_{rvs}$ magnitudes for most sources with radial velocities, and a line broadening parameter is listed for a subset of these. Mean Gaia spectra are made available to the community. The GDR3 catalogue includes about 1 million mean spectra from the radial velocity spectrometer, and about 220 million low-resolution blue and red prism photometer BPRP mean spectra. The results of the analysis of epoch photometry are provided for some 10 million sources across 24 variability types. GDR3 includes astrophysical parameters and source class probabilities for about 470 million and 1500 million sources, respectively, including stars, galaxies, and quasars. Orbital elements and trend parameters are provided for some $800\,000$ astrometric, spectroscopic and eclipsing binaries. More than $150\,000$ Solar System objects, including new discoveries, with preliminary orbital solutions and individual epoch observations are part of this release. Reflectance spectra derived from the epoch BPRP spectral data are published for about 60\,000 asteroids. Finally, an additional data set is provided, namely the Gaia Andromeda Photometric Survey (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00211v1-abstract-full').style.display = 'none'; document.getElementById('2208.00211v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 2 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.12174">arXiv:2206.12174</a> <span> [<a href="https://arxiv.org/pdf/2206.12174">pdf</a>, <a href="https://arxiv.org/format/2206.12174">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243791">10.1051/0004-6361/202243791 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Reflectance spectra of Solar System small bodies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Galluccio%2C+L">L. Galluccio</a>, <a href="/search/astro-ph?searchtype=author&query=Delbo%2C+M">M. Delbo</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Pauwels%2C+T">T. Pauwels</a>, <a href="/search/astro-ph?searchtype=author&query=Tanga%2C+P">P. Tanga</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Cellino%2C+A">A. Cellino</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Muinonen%2C+K">K. Muinonen</a>, <a href="/search/astro-ph?searchtype=author&query=Penttila%2C+A">A. Penttila</a>, <a href="/search/astro-ph?searchtype=author&query=Jordan%2C+S">S. Jordan</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+R">R. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a> , et al. (422 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.12174v1-abstract-short" style="display: inline;"> The Gaia mission of the European Space Agency (ESA) has been routinely observing Solar System objects (SSOs) since the beginning of its operations in August 2014. The Gaia data release three (DR3) includes, for the first time, the mean reflectance spectra of a selected sample of 60 518 SSOs, primarily asteroids, observed between August 5, 2014, and May 28, 2017. Each reflectance spectrum was deriv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.12174v1-abstract-full').style.display = 'inline'; document.getElementById('2206.12174v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.12174v1-abstract-full" style="display: none;"> The Gaia mission of the European Space Agency (ESA) has been routinely observing Solar System objects (SSOs) since the beginning of its operations in August 2014. The Gaia data release three (DR3) includes, for the first time, the mean reflectance spectra of a selected sample of 60 518 SSOs, primarily asteroids, observed between August 5, 2014, and May 28, 2017. Each reflectance spectrum was derived from measurements obtained by means of the Blue and Red photometers (BP/RP), which were binned in 16 discrete wavelength bands. We describe the processing of the Gaia spectral data of SSOs, explaining both the criteria used to select the subset of asteroid spectra published in Gaia DR3, and the different steps of our internal validation procedures. In order to further assess the quality of Gaia SSO reflectance spectra, we carried out external validation against SSO reflectance spectra obtained from ground-based and space-borne telescopes and available in the literature. For each selected SSO, an epoch reflectance was computed by dividing the calibrated spectrum observed by the BP/RP at each transit on the focal plane by the mean spectrum of a solar analogue. The latter was obtained by averaging the Gaia spectral measurements of a selected sample of stars known to have very similar spectra to that of the Sun. Finally, a mean of the epoch reflectance spectra was calculated in 16 spectral bands for each SSO. The agreement between Gaia mean reflectance spectra and those available in the literature is good for bright SSOs, regardless of their taxonomic spectral class. We identify an increase in the spectral slope of S-type SSOs with increasing phase angle. Moreover, we show that the spectral slope increases and the depth of the 1 um absorption band decreases for increasing ages of S-type asteroid families. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.12174v1-abstract-full').style.display = 'none'; document.getElementById('2206.12174v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 26 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.10172">arXiv:2206.10172</a> <span> [<a href="https://arxiv.org/pdf/2206.10172">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.icarus.2022.115012">10.1016/j.icarus.2022.115012 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating S-type asteroid surfaces through reflectance spectra of Ordinary Chondrites </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Eschrig%2C+J">J. Eschrig</a>, <a href="/search/astro-ph?searchtype=author&query=Bonal%2C+L">L. Bonal</a>, <a href="/search/astro-ph?searchtype=author&query=Mahlke%2C+M">M. Mahlke</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+P">P. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Gattacceca%2C+J">J. Gattacceca</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.10172v1-abstract-short" style="display: inline;"> We present an in-depth study of the reflectance spectra of 39 equilibrated and 41 unequilibrated ordinary chondrites. We demonstrate that consistent measuring conditions are vital for the direct comparison of spectral features between chondrites, otherwise hampering any conclusions. We include a comparison with a total of 466 S-type asteroid reflectance spectra. We analyze (i) if a difference betw… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.10172v1-abstract-full').style.display = 'inline'; document.getElementById('2206.10172v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.10172v1-abstract-full" style="display: none;"> We present an in-depth study of the reflectance spectra of 39 equilibrated and 41 unequilibrated ordinary chondrites. We demonstrate that consistent measuring conditions are vital for the direct comparison of spectral features between chondrites, otherwise hampering any conclusions. We include a comparison with a total of 466 S-type asteroid reflectance spectra. We analyze (i) if a difference between EOCs and UOCs as well as between H, L and LL can be seen, (ii) if it is possible to identify unequilibrated and equilibrated S-type asteroid surfaces and (iii) if we can further constrain the match between OCs and S-type asteroids all based on reflectance spectra. We checked the classification of the 31 Antarctic UOCs analyzed in the present work, using petrography and magnetic measurements, and evidenced that 74% of them were misclassified. Reflectance spectra were compared between EOCs and UOCs as well as between H, L and LL chondrites using a set of spectral features including band depths and positions, peak reflectance values, spectral slopes and the Ol/(Ol + Px) ratio. UOCs and EOCs reflectance spectra show no clear-cut dichotomy, but a continuum with some EOCs showing stronger absorption bands and peak reflectance values, while others are comparable to UOCs. We show by the example of 6 EOCs that their band depths decrease with decreasing grain size. Based on reflectance spectra alone, it is thus highly challenging to objectively identify an unequilibrated from an equilibrated S-type surface. There is no clear distinction of the chemical groups: only LL EOCs of petrographic type > 4 can be distinguished from H and L through less deep 2-mic band depths and 1-mic band positions at longer wavelengths. Lastly, an anti-correlation between the diameter of the asteroids and their 1000 nm band depth is found indicating that larger sized S-type asteroids show finer grained surfaces. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.10172v1-abstract-full').style.display = 'none'; document.getElementById('2206.10172v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.06207">arXiv:2206.06207</a> <span> [<a href="https://arxiv.org/pdf/2206.06207">pdf</a>, <a href="https://arxiv.org/format/2206.06207">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243797">10.1051/0004-6361/202243797 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Mapping the asymmetric disc of the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Drimmel%2C+R">R. Drimmel</a>, <a href="/search/astro-ph?searchtype=author&query=Romero-Gomez%2C+M">M. Romero-Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+P">P. Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Poggio%2C+E">E. Poggio</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">R. Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Ginard%2C+A">A. Castro-Ginard</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Figueras%2C+F">F. Figueras</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">M. Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Fremat%2C+Y">Y. Fremat</a>, <a href="/search/astro-ph?searchtype=author&query=Jardine%2C+K">K. Jardine</a>, <a href="/search/astro-ph?searchtype=author&query=Khanna%2C+S">S. Khanna</a>, <a href="/search/astro-ph?searchtype=author&query=Lobel%2C+A">A. Lobel</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+D+J">D. J. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Muraveva%2C+T">T. Muraveva</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a> , et al. (431 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.06207v3-abstract-short" style="display: inline;"> With the most recent Gaia data release the number of sources with complete 6D phase space information (position and velocity) has increased to well over 33 million stars, while stellar astrophysical parameters are provided for more than 470 million sources, in addition to the identification of over 11 million variable stars. Using the astrophysical parameters and variability classifications provid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06207v3-abstract-full').style.display = 'inline'; document.getElementById('2206.06207v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.06207v3-abstract-full" style="display: none;"> With the most recent Gaia data release the number of sources with complete 6D phase space information (position and velocity) has increased to well over 33 million stars, while stellar astrophysical parameters are provided for more than 470 million sources, in addition to the identification of over 11 million variable stars. Using the astrophysical parameters and variability classifications provided in Gaia DR3, we select various stellar populations to explore and identify non-axisymmetric features in the disc of the Milky Way in both configuration and velocity space. Using more about 580 thousand sources identified as hot OB stars, together with 988 known open clusters younger than 100 million years, we map the spiral structure associated with star formation 4-5 kpc from the Sun. We select over 2800 Classical Cepheids younger than 200 million years, which show spiral features extending as far as 10 kpc from the Sun in the outer disc. We also identify more than 8.7 million sources on the red giant branch (RGB), of which 5.7 million have line-of-sight velocities, allowing the velocity field of the Milky Way to be mapped as far as 8 kpc from the Sun, including the inner disc. The spiral structure revealed by the young populations is consistent with recent results using Gaia EDR3 astrometry and source lists based on near infrared photometry, showing the Local (Orion) arm to be at least 8 kpc long, and an outer arm consistent with what is seen in HI surveys, which seems to be a continuation of the Perseus arm into the third quadrant. Meanwhile, the subset of RGB stars with velocities clearly reveals the large scale kinematic signature of the bar in the inner disc, as well as evidence of streaming motions in the outer disc that might be associated with spiral arms or bar resonances. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06207v3-abstract-full').style.display = 'none'; document.getElementById('2206.06207v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 27 figures, accepted for publication in A&A special Gaia DR3 issue. V2: abstract completed. V3: complete author list and link to data: https://drive.google.com/drive/u/1/folders/1yOJPjYmM7QK5XVsqaiSOTuwDQNti2LlZ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A37 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.06075">arXiv:2206.06075</a> <span> [<a href="https://arxiv.org/pdf/2206.06075">pdf</a>, <a href="https://arxiv.org/format/2206.06075">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243767">10.1051/0004-6361/202243767 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Pulsations in main sequence OBAF-type stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=De+Ridder%2C+J">J. De Ridder</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">C. Aerts</a>, <a href="/search/astro-ph?searchtype=author&query=Palaversa%2C+L">L. Palaversa</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</a>, <a href="/search/astro-ph?searchtype=author&query=Audard%2C+M">M. Audard</a>, <a href="/search/astro-ph?searchtype=author&query=Rimoldini%2C+L">L. Rimoldini</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+R">R. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U+L">U. L. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a> , et al. (423 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.06075v2-abstract-short" style="display: inline;"> The third Gaia data release provides photometric time series covering 34 months for about 10 million stars. For many of those stars, a characterisation in Fourier space and their variability classification are also provided. This paper focuses on intermediate- to high-mass (IHM) main sequence pulsators M >= 1.3 Msun) of spectral types O, B, A, or F, known as beta Cep, slowly pulsating B (SPB), del… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06075v2-abstract-full').style.display = 'inline'; document.getElementById('2206.06075v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.06075v2-abstract-full" style="display: none;"> The third Gaia data release provides photometric time series covering 34 months for about 10 million stars. For many of those stars, a characterisation in Fourier space and their variability classification are also provided. This paper focuses on intermediate- to high-mass (IHM) main sequence pulsators M >= 1.3 Msun) of spectral types O, B, A, or F, known as beta Cep, slowly pulsating B (SPB), delta Sct, and gamma Dor stars. These stars are often multi-periodic and display low amplitudes, making them challenging targets to analyse with sparse time series. All datasets used in this analysis are part of the Gaia DR3 data release. The photometric time series were used to perform a Fourier analysis, while the global astrophysical parameters necessary for the empirical instability strips were taken from the Gaia DR3 gspphot tables, and the vsini data were taken from the Gaia DR3 esphs tables. We show that for nearby OBAF-type pulsators, the Gaia DR3 data are precise and accurate enough to pinpoint them in the Hertzsprung-Russell diagram. We find empirical instability strips covering broader regions than theoretically predicted. In particular, our study reveals the presence of fast rotating gravity-mode pulsators outside the strips, as well as the co-existence of rotationally modulated variables inside the strips as reported before in the literature. We derive an extensive period-luminosity relation for delta Sct stars and provide evidence that the relation features different regimes depending on the oscillation period. Finally, we demonstrate how stellar rotation attenuates the amplitude of the dominant oscillation mode of delta Sct stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06075v2-abstract-full').style.display = 'none'; document.getElementById('2206.06075v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A36 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05870">arXiv:2206.05870</a> <span> [<a href="https://arxiv.org/pdf/2206.05870">pdf</a>, <a href="https://arxiv.org/format/2206.05870">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243800">10.1051/0004-6361/202243800 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: A Golden Sample of Astrophysical Parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Sarro%2C+L+M">L. M. Sarro</a>, <a href="/search/astro-ph?searchtype=author&query=Lobel%2C+A">A. Lobel</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">R. Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R+L">R. L. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">M. Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Fr%C3%A9mat%2C+Y">Y. Fr茅mat</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+D+L">D. L. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Th%C3%A9venin%2C+F">F. Th茅venin</a>, <a href="/search/astro-ph?searchtype=author&query=Reyl%C3%A9%2C+C">C. Reyl茅</a>, <a href="/search/astro-ph?searchtype=author&query=Sordo%2C+R">R. Sordo</a>, <a href="/search/astro-ph?searchtype=author&query=Garofalo%2C+A">A. Garofalo</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a> , et al. (423 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.05870v1-abstract-short" style="display: inline;"> Gaia Data Release 3 (DR3) provides a wealth of new data products for the astronomical community to exploit, including astrophysical parameters for a half billion stars. In this work we demonstrate the high quality of these data products and illustrate their use in different astrophysical contexts. We query the astrophysical parameter tables along with other tables in Gaia DR3 to derive the samples… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05870v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05870v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05870v1-abstract-full" style="display: none;"> Gaia Data Release 3 (DR3) provides a wealth of new data products for the astronomical community to exploit, including astrophysical parameters for a half billion stars. In this work we demonstrate the high quality of these data products and illustrate their use in different astrophysical contexts. We query the astrophysical parameter tables along with other tables in Gaia DR3 to derive the samples of the stars of interest. We validate our results by using the Gaia catalogue itself and by comparison with external data. We have produced six homogeneous samples of stars with high quality astrophysical parameters across the HR diagram for the community to exploit. We first focus on three samples that span a large parameter space: young massive disk stars (~3M), FGKM spectral type stars (~3M), and UCDs (~20K). We provide these sources along with additional information (either a flag or complementary parameters) as tables that are made available in the Gaia archive. We furthermore identify 15740 bone fide carbon stars, 5863 solar-analogues, and provide the first homogeneous set of stellar parameters of the Spectro Photometric Standard Stars. We use a subset of the OBA sample to illustrate its usefulness to analyse the Milky Way rotation curve. We then use the properties of the FGKM stars to analyse known exoplanet systems. We also analyse the ages of some unseen UCD-companions to the FGKM stars. We additionally predict the colours of the Sun in various passbands (Gaia, 2MASS, WISE) using the solar-analogue sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05870v1-abstract-full').style.display = 'none'; document.getElementById('2206.05870v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, (incl 6 pages references, acknowledgements, affiliations), 37 figures, A&A accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A39 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05681">arXiv:2206.05681</a> <span> [<a href="https://arxiv.org/pdf/2206.05681">pdf</a>, <a href="https://arxiv.org/format/2206.05681">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243232">10.1051/0004-6361/202243232 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: The extragalactic content </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Bailer-Jones%2C+C+A+L">C. A. L. Bailer-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Teyssier%2C+D">D. Teyssier</a>, <a href="/search/astro-ph?searchtype=author&query=Delchambre%2C+L">L. Delchambre</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Garabato%2C+D">D. Garabato</a>, <a href="/search/astro-ph?searchtype=author&query=Hatzidimitriou%2C+D">D. Hatzidimitriou</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Rimoldini%2C+L">L. Rimoldini</a>, <a href="/search/astro-ph?searchtype=author&query=Bellas-Velidis%2C+I">I. Bellas-Velidis</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo%2C+R">R. Carballo</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Diener%2C+C">C. Diener</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">M. Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Galluccio%2C+L">L. Galluccio</a>, <a href="/search/astro-ph?searchtype=author&query=Gavras%2C+P">P. Gavras</a>, <a href="/search/astro-ph?searchtype=author&query=Krone-Martins%2C+A">A. Krone-Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Teixeira%2C+R">R. Teixeira</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a> , et al. (422 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.05681v1-abstract-short" style="display: inline;"> The Gaia Galactic survey mission is designed and optimized to obtain astrometry, photometry, and spectroscopy of nearly two billion stars in our Galaxy. Yet as an all-sky multi-epoch survey, Gaia also observes several million extragalactic objects down to a magnitude of G~21 mag. Due to the nature of the Gaia onboard selection algorithms, these are mostly point-source-like objects. Using data prov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05681v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05681v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05681v1-abstract-full" style="display: none;"> The Gaia Galactic survey mission is designed and optimized to obtain astrometry, photometry, and spectroscopy of nearly two billion stars in our Galaxy. Yet as an all-sky multi-epoch survey, Gaia also observes several million extragalactic objects down to a magnitude of G~21 mag. Due to the nature of the Gaia onboard selection algorithms, these are mostly point-source-like objects. Using data provided by the satellite, we have identified quasar and galaxy candidates via supervised machine learning methods, and estimate their redshifts using the low resolution BP/RP spectra. We further characterise the surface brightness profiles of host galaxies of quasars and of galaxies from pre-defined input lists. Here we give an overview of the processing of extragalactic objects, describe the data products in Gaia DR3, and analyse their properties. Two integrated tables contain the main results for a high completeness, but low purity (50-70%), set of 6.6 million candidate quasars and 4.8 million candidate galaxies. We provide queries that select purer sub-samples of these containing 1.9 million probable quasars and 2.9 million probable galaxies (both 95% purity). We also use high quality BP/RP spectra of 43 thousand high probability quasars over the redshift range 0.05-4.36 to construct a composite quasar spectrum spanning restframe wavelengths from 72-100 nm. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05681v1-abstract-full').style.display = 'none'; document.getElementById('2206.05681v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05595">arXiv:2206.05595</a> <span> [<a href="https://arxiv.org/pdf/2206.05595">pdf</a>, <a href="https://arxiv.org/format/2206.05595">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243782">10.1051/0004-6361/202243782 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Stellar multiplicity, a teaser for the hidden treasure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Barstow%2C+M+A">M. A. Barstow</a>, <a href="/search/astro-ph?searchtype=author&query=Faigler%2C+S">S. Faigler</a>, <a href="/search/astro-ph?searchtype=author&query=Jorissen%2C+A">A. Jorissen</a>, <a href="/search/astro-ph?searchtype=author&query=Kervella%2C+P">P. Kervella</a>, <a href="/search/astro-ph?searchtype=author&query=Mazeh%2C+T">T. Mazeh</a>, <a href="/search/astro-ph?searchtype=author&query=Mowlavi%2C+N">N. Mowlavi</a>, <a href="/search/astro-ph?searchtype=author&query=Panuzzo%2C+P">P. Panuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Sahlmann%2C+J">J. Sahlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Shahaf%2C+S">S. Shahaf</a>, <a href="/search/astro-ph?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bauchet%2C+N">N. Bauchet</a>, <a href="/search/astro-ph?searchtype=author&query=Damerdji%2C+Y">Y. Damerdji</a>, <a href="/search/astro-ph?searchtype=author&query=Gavras%2C+P">P. Gavras</a>, <a href="/search/astro-ph?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/astro-ph?searchtype=author&query=Gosset%2C+E">E. Gosset</a>, <a href="/search/astro-ph?searchtype=author&query=Halbwachs%2C+J+-">J. -L. Halbwachs</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</a>, <a href="/search/astro-ph?searchtype=author&query=Lattanzi%2C+M+G">M. G. Lattanzi</a>, <a href="/search/astro-ph?searchtype=author&query=Leclerc%2C+N">N. Leclerc</a>, <a href="/search/astro-ph?searchtype=author&query=Morel%2C+T">T. Morel</a>, <a href="/search/astro-ph?searchtype=author&query=Pourbaix%2C+D">D. Pourbaix</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorentin%2C+P+R">P. Re Fiorentin</a> , et al. (425 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.05595v1-abstract-short" style="display: inline;"> The Gaia DR3 Catalogue contains for the first time about eight hundred thousand solutions with either orbital elements or trend parameters for astrometric, spectroscopic and eclipsing binaries, and combinations of them. This paper aims to illustrate the huge potential of this large non-single star catalogue. Using the orbital solutions together with models of the binaries, a catalogue of tens of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05595v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05595v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05595v1-abstract-full" style="display: none;"> The Gaia DR3 Catalogue contains for the first time about eight hundred thousand solutions with either orbital elements or trend parameters for astrometric, spectroscopic and eclipsing binaries, and combinations of them. This paper aims to illustrate the huge potential of this large non-single star catalogue. Using the orbital solutions together with models of the binaries, a catalogue of tens of thousands of stellar masses, or lower limits, partly together with consistent flux ratios, has been built. Properties concerning the completeness of the binary catalogues are discussed, statistical features of the orbital elements are explained and a comparison with other catalogues is performed. Illustrative applications are proposed for binaries across the H-R diagram. The binarity is studied in the RGB/AGB and a search for genuine SB1 among long-period variables is performed. The discovery of new EL CVn systems illustrates the potential of combining variability and binarity catalogues. Potential compact object companions are presented, mainly white dwarf companions or double degenerates, but one candidate neutron star is also presented. Towards the bottom of the main sequence, the orbits of previously-suspected binary ultracool dwarfs are determined and new candidate binaries are discovered. The long awaited contribution of Gaia to the analysis of the substellar regime shows the brown dwarf desert around solar-type stars using true, rather than minimum, masses, and provides new important constraints on the occurrence rates of substellar companions to M dwarfs. Several dozen new exoplanets are proposed, including two with validated orbital solutions and one super-Jupiter orbiting a white dwarf, all being candidates requiring confirmation. Beside binarity, higher order multiple systems are also found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05595v1-abstract-full').style.display = 'none'; document.getElementById('2206.05595v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">60 pages, 60 figures. Accepted for publication in Astronomy & Astrophysics (2022-06-09). The catalogue of binary masses is available for download from the ESA Gaia DR3 Archive and will be available from the CDS/VizieR service</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A34 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05561">arXiv:2206.05561</a> <span> [<a href="https://arxiv.org/pdf/2206.05561">pdf</a>, <a href="https://arxiv.org/format/2206.05561">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243796">10.1051/0004-6361/202243796 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Data Release 3: the Solar System survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tanga%2C+P">P. Tanga</a>, <a href="/search/astro-ph?searchtype=author&query=Pauwels%2C+T">T. Pauwels</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Muinonen%2C+K">K. Muinonen</a>, <a href="/search/astro-ph?searchtype=author&query=Cellino%2C+A">A. Cellino</a>, <a href="/search/astro-ph?searchtype=author&query=David%2C+P">P. David</a>, <a href="/search/astro-ph?searchtype=author&query=Hestroffer%2C+D">D. Hestroffer</a>, <a href="/search/astro-ph?searchtype=author&query=Spoto%2C+F">F. Spoto</a>, <a href="/search/astro-ph?searchtype=author&query=Berthier%2C+J">J. Berthier</a>, <a href="/search/astro-ph?searchtype=author&query=Guiraud%2C+J">J. Guiraud</a>, <a href="/search/astro-ph?searchtype=author&query=Roux%2C+W">W. Roux</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Delbo%2C+M">M. Delbo</a>, <a href="/search/astro-ph?searchtype=author&query=Oro%2C+A+D">A. Dell Oro</a>, <a href="/search/astro-ph?searchtype=author&query=Fouron%2C+C">C. Fouron</a>, <a href="/search/astro-ph?searchtype=author&query=Galluccio%2C+L">L. Galluccio</a>, <a href="/search/astro-ph?searchtype=author&query=Jonckheere%2C+A">A. Jonckheere</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Lefustec%2C+Y">Y. Lefustec</a>, <a href="/search/astro-ph?searchtype=author&query=Liberato%2C+L">L. Liberato</a>, <a href="/search/astro-ph?searchtype=author&query=Ord%C3%A9novic%2C+C">C. Ord茅novic</a>, <a href="/search/astro-ph?searchtype=author&query=Oreshina-Slezak%2C+I">I. Oreshina-Slezak</a>, <a href="/search/astro-ph?searchtype=author&query=Penttil%C3%A4%2C+A">A. Penttil盲</a>, <a href="/search/astro-ph?searchtype=author&query=Pailler%2C+F">F. Pailler</a>, <a href="/search/astro-ph?searchtype=author&query=Panem%2C+C">Ch. Panem</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.05561v1-abstract-short" style="display: inline;"> The third data release by the Gaia mission of the European Space (DR3) is the first release to provide the community with a large sample of observations for more than 150 thousand Solar System objects, including asteroids and natural planetary satellites. The release contains astrometry (over 23 million epochs) and photometry, along with average reflectance spectra of 60518 asteroids and osculatin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05561v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05561v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05561v1-abstract-full" style="display: none;"> The third data release by the Gaia mission of the European Space (DR3) is the first release to provide the community with a large sample of observations for more than 150 thousand Solar System objects, including asteroids and natural planetary satellites. The release contains astrometry (over 23 million epochs) and photometry, along with average reflectance spectra of 60518 asteroids and osculating elements. We present an overview of the procedures that have been implemented over several years of development and tests to process Solar System data at the level of accuracy that Gaia can reach. We illustrate the data properties and potential with some practical examples. In order to allow the users of DR3 to best exploit the data, we explain the assumptions and approaches followed in the implementation of the data processing pipeline for Solar System processing, and their effects in terms of data filtering, optimisation, and performances. We then test the data quality by analysing post-fit residuals to adjusted orbits, the capacity of detecting subtle dynamical effects (wobbling due to satellites or shape and Yarkovsky acceleration), and to reproduce known properties of asteroid photometry (phase curves and rotational light curves). The DR3 astrometric accuracy is a clear improvement over the data published in DR2, which concerned a very limited sample of asteroids. The performance of the data reduction is met, and is illustrated by the capacity of detecting milliarcsecond-level wobbling of the asteroid photocentre that is due to satellite or shape effects and contributes to Yarkovsky effect measurements. The third data release can in terms of data completeness and accuracy be considered the first full-scale realisation of the Solar System survey by Gaia. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05561v1-abstract-full').style.display = 'none'; document.getElementById('2206.05561v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Gaia DR3 article</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy and Astrophysics 2022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05534">arXiv:2206.05534</a> <span> [<a href="https://arxiv.org/pdf/2206.05534">pdf</a>, <a href="https://arxiv.org/format/2206.05534">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243511">10.1051/0004-6361/202243511 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Chemical cartography of the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Recio-Blanco%2C+A">A. Recio-Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">G. Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=de+Laverny%2C+P">P. de Laverny</a>, <a href="/search/astro-ph?searchtype=author&query=Palicio%2C+P+A">P. A. Palicio</a>, <a href="/search/astro-ph?searchtype=author&query=Spagna%2C+A">A. Spagna</a>, <a href="/search/astro-ph?searchtype=author&query=Spina%2C+L">L. Spina</a>, <a href="/search/astro-ph?searchtype=author&query=Katz%2C+D">D. Katz</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorentin%2C+P+R">P. Re Fiorentin</a>, <a href="/search/astro-ph?searchtype=author&query=Poggio%2C+E">E. Poggio</a>, <a href="/search/astro-ph?searchtype=author&query=McMillan%2C+P+J">P. J. McMillan</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Lattanzi%2C+M+G">M. G. Lattanzi</a>, <a href="/search/astro-ph?searchtype=author&query=Seabroke%2C+G+M">G. M. Seabroke</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Antoja%2C+T">T. Antoja</a>, <a href="/search/astro-ph?searchtype=author&query=Bailer-Jones%2C+C+A+L">C. A. L. Bailer-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">R. Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">M. Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Cropper%2C+M">M. Cropper</a>, <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Bijaoui%2C+A">A. Bijaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a> , et al. (425 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.05534v1-abstract-short" style="display: inline;"> Gaia DR3 opens a new era of all-sky spectral analysis of stellar populations thanks to the nearly 5.6 million stars observed by the RVS and parametrised by the GSP-spec module. The all-sky Gaia chemical cartography allows a powerful and precise chemo-dynamical view of the Milky Way with unprecedented spatial coverage and statistical robustness. First, it reveals the strong vertical symmetry of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05534v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05534v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05534v1-abstract-full" style="display: none;"> Gaia DR3 opens a new era of all-sky spectral analysis of stellar populations thanks to the nearly 5.6 million stars observed by the RVS and parametrised by the GSP-spec module. The all-sky Gaia chemical cartography allows a powerful and precise chemo-dynamical view of the Milky Way with unprecedented spatial coverage and statistical robustness. First, it reveals the strong vertical symmetry of the Galaxy and the flared structure of the disc. Second, the observed kinematic disturbances of the disc -- seen as phase space correlations -- and kinematic or orbital substructures are associated with chemical patterns that favour stars with enhanced metallicities and lower [alpha/Fe] abundance ratios compared to the median values in the radial distributions. This is detected both for young objects that trace the spiral arms and older populations. Several alpha, iron-peak elements and at least one heavy element trace the thin and thick disc properties in the solar cylinder. Third, young disc stars show a recent chemical impoverishment in several elements. Fourth, the largest chemo-dynamical sample of open clusters analysed so far shows a steepening of the radial metallicity gradient with age, which is also observed in the young field population. Finally, the Gaia chemical data have the required coverage and precision to unveil galaxy accretion debris and heated disc stars on halo orbits through their [alpha/Fe] ratio, and to allow the study of the chemo-dynamical properties of globular clusters. Gaia DR3 chemo-dynamical diagnostics open new horizons before the era of ground-based wide-field spectroscopic surveys. They unveil a complex Milky Way that is the outcome of an eventful evolution, shaping it to the present day (abridged). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05534v1-abstract-full').style.display = 'none'; document.getElementById('2206.05534v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astronomy and Astrophysics (accepted, in press)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A38 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.12574">arXiv:2204.12574</a> <span> [<a href="https://arxiv.org/pdf/2204.12574">pdf</a>, <a href="https://arxiv.org/format/2204.12574">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243483">10.1051/0004-6361/202243483 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: The celestial reference frame (Gaia-CRF3) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">J. Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Lerate%2C+M">M. Ramos-Lerate</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+U">U. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Bombrun%2C+A">A. Bombrun</a>, <a href="/search/astro-ph?searchtype=author&query=de+Torres%2C+A">A. de Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Gerlach%2C+E">E. Gerlach</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+R">R. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hilger%2C+T">T. Hilger</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+D">D. Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U+L">U. L. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=McMillan%2C+P+J">P. J. McMillan</a>, <a href="/search/astro-ph?searchtype=author&query=Steidelm%C3%BCller%2C+H">H. Steidelm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Teyssier%2C+D">D. Teyssier</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Bartolom%C3%A9%2C+S">S. Bartolom茅</a>, <a href="/search/astro-ph?searchtype=author&query=Bernet%2C+M">M. Bernet</a>, <a href="/search/astro-ph?searchtype=author&query=Casta%C3%B1eda%2C+J">J. Casta帽eda</a>, <a href="/search/astro-ph?searchtype=author&query=Clotet%2C+M">M. Clotet</a>, <a href="/search/astro-ph?searchtype=author&query=Davidson%2C+M">M. Davidson</a>, <a href="/search/astro-ph?searchtype=author&query=Fabricius%2C+C">C. Fabricius</a> , et al. (426 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.12574v2-abstract-short" style="display: inline;"> Gaia-CRF3 is the celestial reference frame for positions and proper motions in the third release of data from the Gaia mission, Gaia DR3 (and for the early third release, Gaia EDR3, which contains identical astrometric results). The reference frame is defined by the positions and proper motions at epoch 2016.0 for a specific set of extragalactic sources in the (E)DR3 catalogue. We describe the c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.12574v2-abstract-full').style.display = 'inline'; document.getElementById('2204.12574v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.12574v2-abstract-full" style="display: none;"> Gaia-CRF3 is the celestial reference frame for positions and proper motions in the third release of data from the Gaia mission, Gaia DR3 (and for the early third release, Gaia EDR3, which contains identical astrometric results). The reference frame is defined by the positions and proper motions at epoch 2016.0 for a specific set of extragalactic sources in the (E)DR3 catalogue. We describe the construction of Gaia-CRF3, and its properties in terms of the distributions in magnitude, colour, and astrometric quality. Compact extragalactic sources in Gaia DR3 were identified by positional cross-matching with 17 external catalogues of quasars (QSO) and active galactic nuclei (AGN), followed by astrometric filtering designed to remove stellar contaminants. Selecting a clean sample was favoured over including a higher number of extragalactic sources. For the final sample, the random and systematic errors in the proper motions are analysed, as well as the radio-optical offsets in position for sources in the third realisation of the International Celestial Reference Frame (ICRF3). The Gaia-CRF3 comprises about 1.6 million QSO-like sources, of which 1.2 million have five-parameter astrometric solutions in Gaia DR3 and 0.4 million have six-parameter solutions. The sources span the magnitude range G = 13 to 21 with a peak density at 20.6 mag, at which the typical positional uncertainty is about 1 mas. The proper motions show systematic errors on the level of 12 $渭$as yr${}^{-1}$ on angular scales greater than 15 deg. For the 3142 optical counterparts of ICRF3 sources in the S/X frequency bands, the median offset from the radio positions is about 0.5 mas, but exceeds 4 mas in either coordinate for 127 sources. We outline the future of the Gaia-CRF in the next Gaia data releases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.12574v2-abstract-full').style.display = 'none'; document.getElementById('2204.12574v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 667, A148 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.11229">arXiv:2203.11229</a> <span> [<a href="https://arxiv.org/pdf/2203.11229">pdf</a>, <a href="https://arxiv.org/format/2203.11229">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243587">10.1051/0004-6361/202243587 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Asteroid Taxonomy from Cluster Analysis of Spectrometry and Albedo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mahlke%2C+M">Max Mahlke</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Mattei%2C+P">Pierre-Alexandre Mattei</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.11229v2-abstract-short" style="display: inline;"> The classification of the minor bodies of the Solar System based on observables has been continuously developed and iterated over the past 40 years. While prior iterations followed either the availability of large observational campaigns or new instrumental capabilities opening new observational dimensions, we see the opportunity to improve primarily upon the established methodology. We develope… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.11229v2-abstract-full').style.display = 'inline'; document.getElementById('2203.11229v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.11229v2-abstract-full" style="display: none;"> The classification of the minor bodies of the Solar System based on observables has been continuously developed and iterated over the past 40 years. While prior iterations followed either the availability of large observational campaigns or new instrumental capabilities opening new observational dimensions, we see the opportunity to improve primarily upon the established methodology. We developed an iteration of the asteroid taxonomy which allows the classification of partial and complete observations (i.e. visible, near-infrared, and visible-near-infrared spectrometry) and which reintroduces the visual albedo into the classification observables. The resulting class assignments are given probabilistically, enabling the uncertainty of a classification to be quantified. We built the taxonomy based on 2983 observations of 2125 individual asteroids, representing an almost tenfold increase of sample size compared with the previous taxonomy. The asteroid classes are identified in a lower-dimensional representation of the observations using a mixture of common factor analysers model. We identify 17 classes split into the three complexes C, M, and S, including the new Z-class for extremely-red objects in the main belt. The visual albedo information resolves the spectral degeneracy of the X-complex and establishes the P-class as part of the C-complex. We present a classification tool which computes probabilistic class assignments within this taxonomic scheme from asteroid observations. The taxonomic classifications of 6038 observations of 4526 individual asteroids are published. The ability to classify partial observations and the reintroduction of the visual albedo provide a taxonomy which is well suited for the current and future datasets of asteroid observations, in particular provided by the Gaia, MITHNEOS, NEO Surveyor, and SPHEREx surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.11229v2-abstract-full').style.display = 'none'; document.getElementById('2203.11229v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Astronomy and Astrophysics. The table of asteroid classifications and the templates of the defined taxonomic classes are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/665/A26</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 665, A26 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.13797">arXiv:2202.13797</a> <span> [<a href="https://arxiv.org/pdf/2202.13797">pdf</a>, <a href="https://arxiv.org/format/2202.13797">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.icarus.2022.114971">10.1016/j.icarus.2022.114971 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Connecting Asteroids and Meteorites with visible and near-infrared spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DeMeo%2C+F+E">Francesca E. DeMeo</a>, <a href="/search/astro-ph?searchtype=author&query=Burt%2C+B+J">Brian J. Burt</a>, <a href="/search/astro-ph?searchtype=author&query=Marsset%2C+M">Micha毛l Marsset</a>, <a href="/search/astro-ph?searchtype=author&query=Polishook%2C+D">David Polishook</a>, <a href="/search/astro-ph?searchtype=author&query=Burbine%2C+T+H">Thomas H. Burbine</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Beno卯t Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Binzel%2C+R+P">Richard P. Binzel</a>, <a href="/search/astro-ph?searchtype=author&query=Vernazza%2C+P">Pierre Vernazza</a>, <a href="/search/astro-ph?searchtype=author&query=Reddy%2C+V">Vishnu Reddy</a>, <a href="/search/astro-ph?searchtype=author&query=Tang%2C+M">Michelle Tang</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+C+A">Cristina A. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Rivkin%2C+A+S">Andrew S. Rivkin</a>, <a href="/search/astro-ph?searchtype=author&query=Moskovitz%2C+N+A">Nicholas A. Moskovitz</a>, <a href="/search/astro-ph?searchtype=author&query=Slivan%2C+S+M">Stephen M. Slivan</a>, <a href="/search/astro-ph?searchtype=author&query=Bus%2C+S+J">Schelte J. Bus</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.13797v1-abstract-short" style="display: inline;"> We identify spectral similarities between asteroids and meteorites. We identify spectral matches between 500 asteroid spectra and over 1,000 samples of RELAB meteorite spectra over 0.45-2.5 microns. We reproduce many major and previously known meteorite-asteroid connections and find possible new, more rare or less-established connections. Well-established connections include: ordinary chondrites (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.13797v1-abstract-full').style.display = 'inline'; document.getElementById('2202.13797v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.13797v1-abstract-full" style="display: none;"> We identify spectral similarities between asteroids and meteorites. We identify spectral matches between 500 asteroid spectra and over 1,000 samples of RELAB meteorite spectra over 0.45-2.5 microns. We reproduce many major and previously known meteorite-asteroid connections and find possible new, more rare or less-established connections. Well-established connections include: ordinary chondrites (OC) with S-complex asteroids; pristine CM carbonaceous chondrites with Ch-type asteroids and heated CMs with C-type asteroids; HED meteorites with V-types; enstatite chondrites with Xc-type asteroids; CV meteorites with K-type asteroids; Brachinites, Pallasites and R chondrites with olivine-dominated A-type asteroids. We find a trend from Q, Sq, S, Sr to Sv correlates with LL to H, with Q-types matching predominately to L and LL ordinary chondrites, and Sr and Sv matching predominantly with L and H ordinary chondrites. Ordinary chondrite samples that match to the X-complex, all measurements of slabs and many labeled as dark or black (shocked) OCs. We find carbonaceous chondrite samples having spectral slopes large enough to match D-type asteroid spectra. In many cases the asteroid type to meteorite type links are not unique. While there are well established matches between an asteroid class and meteorite class, there are less common but still spectrally compatible matches between many asteroid types and meteorite types. This result emphasizes the diversity of asteroid and meteorite compositions and highlights the degeneracy of classification by spectral features alone. Recent and upcoming spacecraft missions will shed light on the compositions of many of the asteroid classes, particularly those without diagnostic features, (C-, B-, X-, and D-types), with measurements of Ceres, Ryugu, Bennu, Psyche, and C-, P-, and D-types as part of the Lucy mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.13797v1-abstract-full').style.display = 'none'; document.getElementById('2202.13797v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Icarus. 38 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.13796">arXiv:2202.13796</a> <span> [<a href="https://arxiv.org/pdf/2202.13796">pdf</a>, <a href="https://arxiv.org/format/2202.13796">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac532f">10.3847/1538-3881/ac532f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The debiased compositional distribution of MITHNEOS: Global match between the near-Earth and main-belt asteroid populations and excess of D-type Near-Earth Objects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marsset%2C+M">Micha毛l Marsset</a>, <a href="/search/astro-ph?searchtype=author&query=DeMeo%2C+F+E">Francesca E. DeMeo</a>, <a href="/search/astro-ph?searchtype=author&query=Burt%2C+B">Brian Burt</a>, <a href="/search/astro-ph?searchtype=author&query=Polishook%2C+D">David Polishook</a>, <a href="/search/astro-ph?searchtype=author&query=Binzel%2C+R+P">Richard P. Binzel</a>, <a href="/search/astro-ph?searchtype=author&query=Granvik%2C+M">Mikael Granvik</a>, <a href="/search/astro-ph?searchtype=author&query=Vernazza%2C+P">Pierre Vernazza</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Bus%2C+S+J">Schelte J. Bus</a>, <a href="/search/astro-ph?searchtype=author&query=Slivan%2C+S+M">Stephen M. Slivan</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+C+A">Cristina A. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Moskovitz%2C+N+A">Nicholas A. Moskovitz</a>, <a href="/search/astro-ph?searchtype=author&query=Rivkin%2C+A+S">Andrew S. Rivkin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.13796v1-abstract-short" style="display: inline;"> We report 491 new near-infrared spectroscopic measurements of 420 near-Earth objects (NEOs) collected on the NASA InfraRed Telescope Facility (IRTF) as part of the MIT-Hawaii NEO Spectroscopic Survey (MITHNEOS). These measurements were combined with previously published data (Binzel et al. 2019) and bias-corrected to derive the intrinsic compositional distribution of the overall NEO population, as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.13796v1-abstract-full').style.display = 'inline'; document.getElementById('2202.13796v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.13796v1-abstract-full" style="display: none;"> We report 491 new near-infrared spectroscopic measurements of 420 near-Earth objects (NEOs) collected on the NASA InfraRed Telescope Facility (IRTF) as part of the MIT-Hawaii NEO Spectroscopic Survey (MITHNEOS). These measurements were combined with previously published data (Binzel et al. 2019) and bias-corrected to derive the intrinsic compositional distribution of the overall NEO population, as well as of subpopulations coming from various escape routes (ERs) in the asteroid belt and beyond. The resulting distributions reflect well the overall compositional gradient of the asteroid belt, with decreasing fractions of silicate-rich (S- and Q-type) bodies and increasing fractions of carbonaceous (B-, C-, D- and P-type) bodies as a function of increasing ER distance from the Sun. The close compositional match between NEOs and their predicted source populations validates dynamical models used to identify ERs and argues against any strong composition change with size in the asteroid belt between ~5 km down to ~100 m. A notable exception comes from the over-abundance of D-type NEOs from the 5:2J and, to a lesser extend, the 3:1J and nu6 ERs, hinting at the presence of a large population of small D-type asteroids in the main belt. Alternatively, this excess may indicate preferential spectral evolution from D-type surfaces to C- and P-types as a consequence of space weathering, or to the fact that D-type objects fragment more often than other spectral types in the NEO space. No further evidence for the existence of collisional families in the main belt, below the detection limit of current main-belt surveys, was found in this work. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.13796v1-abstract-full').style.display = 'none'; document.getElementById('2202.13796v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 6 figures, accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.00246">arXiv:2202.00246</a> <span> [<a href="https://arxiv.org/pdf/2202.00246">pdf</a>, <a href="https://arxiv.org/format/2202.00246">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202142998">10.1051/0004-6361/202142998 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hubble Asteroid Hunter: I. Identifying asteroid trails in Hubble Space Telescope images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S">Sandor Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn%2C+P+G">Pablo Garc铆a Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Popescu%2C+M">Marcel Popescu</a>, <a href="/search/astro-ph?searchtype=author&query=Mer%C3%ADn%2C+B">Bruno Mer铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Mahlke%2C+M">Max Mahlke</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Beno卯t Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Thomson%2C+R">Ross Thomson</a>, <a href="/search/astro-ph?searchtype=author&query=Karadag%2C+S">Samet Karadag</a>, <a href="/search/astro-ph?searchtype=author&query=Dur%C3%A1n%2C+J">Javier Dur谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Racero%2C+E">Elena Racero</a>, <a href="/search/astro-ph?searchtype=author&query=Giordano%2C+F">Fabrizio Giordano</a>, <a href="/search/astro-ph?searchtype=author&query=Baines%2C+D">Deborah Baines</a>, <a href="/search/astro-ph?searchtype=author&query=de+Marchi%2C+G">Guido de Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Laureijs%2C+R">Ren茅 Laureijs</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.00246v2-abstract-short" style="display: inline;"> Large and publicly available astronomical archives open up new possibilities to search and study Solar System objects. However, advanced techniques are required to deal with the large amounts of data. These unbiased surveys can be used to constrain the size distribution of minor bodies, which represents a piece of the puzzle for the formation models of the Solar System. We aim to identify asteroid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.00246v2-abstract-full').style.display = 'inline'; document.getElementById('2202.00246v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.00246v2-abstract-full" style="display: none;"> Large and publicly available astronomical archives open up new possibilities to search and study Solar System objects. However, advanced techniques are required to deal with the large amounts of data. These unbiased surveys can be used to constrain the size distribution of minor bodies, which represents a piece of the puzzle for the formation models of the Solar System. We aim to identify asteroids in archival images from the ESA Hubble Space Telescope (HST) Science data archive using data mining. We developed a citizen science project on the Zooniverse platform, Hubble Asteroid Hunter (www.asteroidhunter.org) asking members of the public to identify asteroid trails in archival HST images. We used the labels provided by the volunteers to train an automated deep learning model built with Google Cloud AutoML Vision to explore the entire HST archive to detect asteroids crossing the field-of-view. We report the detection of 1701 new asteroid trails identified in archival HST data via our citizen science project and the subsequent machine learning exploration of the ESA HST science data archive. We detect asteroids to a magnitude of 24.5, which are statistically fainter than the populations of asteroids identified from ground-based surveys. The majority of asteroids are distributed near the ecliptic plane, as expected, where we find an approximate density of 80 asteroids per square degree. We match 670 trails (39% of the trails found) with 454 known Solar System objects in the Minor Planet Center database, however, no matches are found for 1031 (61%) trails. The unidentified asteroids are faint, being on average 1.6 magnitudes fainter than the asteroids we succeeded to identify. They probably correspond to previously unknown objects. This work demonstrates that citizen science and machine learning are useful techniques for the systematic search of SSOs in existing astronomy science archives. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.00246v2-abstract-full').style.display = 'none'; document.getElementById('2202.00246v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 16 figures, 2 tables. Replaced to match the A&A journal version, https://www.aanda.org/10.1051/0004-6361/202142998</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A85 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.03862">arXiv:2201.03862</a> <span> [<a href="https://arxiv.org/pdf/2201.03862">pdf</a>, <a href="https://arxiv.org/format/2201.03862">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.5281/zenodo.7195671">10.5281/zenodo.7195671 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Rubin-Euclid Derived Data Products: Initial Recommendations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guy%2C+L+P">Leanne P. Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Bachelet%2C+E">Etienne Bachelet</a>, <a href="/search/astro-ph?searchtype=author&query=Banerji%2C+M">Manda Banerji</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Collett%2C+T">Thomas Collett</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Eggl%2C+S">Siegfried Eggl</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A">Annette Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Heymans%2C+C">Catherine Heymans</a>, <a href="/search/astro-ph?searchtype=author&query=Hook%2C+I+M">Isobel M. Hook</a>, <a href="/search/astro-ph?searchtype=author&query=Aubourg%2C+%C3%89">脡ric Aubourg</a>, <a href="/search/astro-ph?searchtype=author&query=Aussel%2C+H">Herv茅 Aussel</a>, <a href="/search/astro-ph?searchtype=author&query=Bosch%2C+J">James Bosch</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Hoekstra%2C+H">Henk Hoekstra</a>, <a href="/search/astro-ph?searchtype=author&query=Kuijken%2C+K">Konrad Kuijken</a>, <a href="/search/astro-ph?searchtype=author&query=Lanusse%2C+F">Francois Lanusse</a>, <a href="/search/astro-ph?searchtype=author&query=Melchior%2C+P">Peter Melchior</a>, <a href="/search/astro-ph?searchtype=author&query=Mohr%2C+J">Joseph Mohr</a>, <a href="/search/astro-ph?searchtype=author&query=Moresco%2C+M">Michele Moresco</a>, <a href="/search/astro-ph?searchtype=author&query=Nakajima%2C+R">Reiko Nakajima</a>, <a href="/search/astro-ph?searchtype=author&query=Paltani%2C+S">St茅phane Paltani</a>, <a href="/search/astro-ph?searchtype=author&query=Troxel%2C+M">Michael Troxel</a> , et al. (95 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.03862v2-abstract-short" style="display: inline;"> This report is the result of a joint discussion between the Rubin and Euclid scientific communities. The work presented in this report was focused on designing and recommending an initial set of Derived Data products (DDPs) that could realize the science goals enabled by joint processing. All interested Rubin and Euclid data rights holders were invited to contribute via an online discussion forum… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03862v2-abstract-full').style.display = 'inline'; document.getElementById('2201.03862v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.03862v2-abstract-full" style="display: none;"> This report is the result of a joint discussion between the Rubin and Euclid scientific communities. The work presented in this report was focused on designing and recommending an initial set of Derived Data products (DDPs) that could realize the science goals enabled by joint processing. All interested Rubin and Euclid data rights holders were invited to contribute via an online discussion forum and a series of virtual meetings. Strong interest in enhancing science with joint DDPs emerged from across a wide range of astrophysical domains: Solar System, the Galaxy, the Local Volume, from the nearby to the primaeval Universe, and cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03862v2-abstract-full').style.display = 'none'; document.getElementById('2201.03862v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Report of the Rubin-Euclid Derived Data Products Working Group, 78 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.13120">arXiv:2111.13120</a> <span> [<a href="https://arxiv.org/pdf/2111.13120">pdf</a>, <a href="https://arxiv.org/format/2111.13120">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140899">10.1051/0004-6361/202140899 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ESASky SSOSS: Solar System Object Search Service and the case of Psyche </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Racero%2C+E">E. Racero</a>, <a href="/search/astro-ph?searchtype=author&query=Giordano%2C+F">F. Giordano</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Berthier%2C+J">J. Berthier</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+T">T. M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Mahlke%2C+M">M. Mahlke</a>, <a href="/search/astro-ph?searchtype=author&query=Valtchanov%2C+I">I. Valtchanov</a>, <a href="/search/astro-ph?searchtype=author&query=Baines%2C+D">D. Baines</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S">S. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Mer%C3%ADn%2C+B">B. Mer铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Besse%2C+S">S. Besse</a>, <a href="/search/astro-ph?searchtype=author&query=K%C3%BCppers%2C+M">M. K眉ppers</a>, <a href="/search/astro-ph?searchtype=author&query=Puga%2C+E">E. Puga</a>, <a href="/search/astro-ph?searchtype=author&query=N%C3%BA%C3%B1ez%2C+J+G">J. Gonz谩lez N煤帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+P">P. Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Calle%2C+I">I. de la Calle</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Mart%C3%AD%2C+B">B. L贸pez-Mart铆</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+H">H. Norman</a>, <a href="/search/astro-ph?searchtype=author&query=Wrangblad%2C+M">M. Wrangblad</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Caniego%2C+M">M. L贸pez-Caniego</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+N+%C3%81">N. 脕lvarez Crespo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.13120v1-abstract-short" style="display: inline;"> We introduce in this work the Solar System Object Search Service (SSOSS), a service aimed at providing the scientific community with a search service for all potential detections of SSOs among the ESA astronomy archival imaging data. We illustrate its functionalities using the case of asteroid (16) Psyche, for which no information in the far-IR (70-500 渭m) has previously been reported, to derive i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.13120v1-abstract-full').style.display = 'inline'; document.getElementById('2111.13120v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.13120v1-abstract-full" style="display: none;"> We introduce in this work the Solar System Object Search Service (SSOSS), a service aimed at providing the scientific community with a search service for all potential detections of SSOs among the ESA astronomy archival imaging data. We illustrate its functionalities using the case of asteroid (16) Psyche, for which no information in the far-IR (70-500 渭m) has previously been reported, to derive its thermal properties in preparation for the upcoming NASA Psyche mission. This service performs a geometrical cross-match of the orbital path of each object with respect to the public high-level imaging footprints stored in the ESA archives. For this first release, three missions were chosen: XMM-Newton, the Hubble Space Telescope (HST), and Herschel Observatory. We present a catalog listing all potential detections of asteroids within estimated limiting magnitude or flux limit in Herschel, XMM-Newton, and HST archival imaging data, including 909 serendipitous detections in Herschel images, 985 in XMM-Newton Optical Monitor camera images, and over 32,000 potential serendipitous detections in HST images. We also present a case study: the analysis of the thermal properties of Psyche from four serendipitous Herschel detections, combined with previously published thermal IR measurements. We see strong evidence for an unusual drop in (hemispherical spectral) emissivity, from 0.9 at 100 渭m down to about 0.6 at 350 渭m, followed by a possible but not well-constrained increase towards 500 渭m, comparable to what was found for Vesta. The combined thermal data set puts a strong constraint on Psyche's thermal inertia (between 20 to 80$J m^{-2} s^{-1/2} K^{-1}$) and favours an intermediate to low level surface roughness (below 0.4 for the rms of surface slopes). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.13120v1-abstract-full').style.display = 'none'; document.getElementById('2111.13120v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 17 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 659, A38 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.12702">arXiv:2110.12702</a> <span> [<a href="https://arxiv.org/pdf/2110.12702">pdf</a>, <a href="https://arxiv.org/format/2110.12702">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202142055">10.1051/0004-6361/202142055 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observed tidal evolution of Kleopatra's outer satellite </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bro%C5%BE%2C+M">M. Bro啪</a>, <a href="/search/astro-ph?searchtype=author&query=%C4%8Eurech%2C+J">J. 膸urech</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Vachier%2C+F">F. Vachier</a>, <a href="/search/astro-ph?searchtype=author&query=Marchis%2C+F">F. Marchis</a>, <a href="/search/astro-ph?searchtype=author&query=Hanu%C5%A1%2C+J">J. Hanu拧</a>, <a href="/search/astro-ph?searchtype=author&query=Jorda%2C+L">L. Jorda</a>, <a href="/search/astro-ph?searchtype=author&query=Vernazza%2C+P">P. Vernazza</a>, <a href="/search/astro-ph?searchtype=author&query=Vokrouhlick%C3%BD%2C+D">D. Vokrouhlick媒</a>, <a href="/search/astro-ph?searchtype=author&query=Walterov%C3%A1%2C+M">M. Walterov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+R">R. Behrend</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.12702v1-abstract-short" style="display: inline;"> The orbit of the outer satellite Alexhelios of (216) Kleopatra is already constrained by adaptive-optics astrometry, obtained with the VLT/SPHERE instrument. However, there is also a preceding occultation event in 1980 attributed to this satellite. Hereinafter, we try to link all observations, spanning 1980--2018. We find the nominal orbit exhibits an unexplained shift by $+60^\circ$ in the true l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.12702v1-abstract-full').style.display = 'inline'; document.getElementById('2110.12702v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.12702v1-abstract-full" style="display: none;"> The orbit of the outer satellite Alexhelios of (216) Kleopatra is already constrained by adaptive-optics astrometry, obtained with the VLT/SPHERE instrument. However, there is also a preceding occultation event in 1980 attributed to this satellite. Hereinafter, we try to link all observations, spanning 1980--2018. We find the nominal orbit exhibits an unexplained shift by $+60^\circ$ in the true longitude. Using both periodogram analysis and an $\ell = 10$ multipole model suitable for the motion of mutually interacting moons about the irregular body, we confirmed that it is not possible to adjust the respective osculating period $P_2$. Instead, we were forced to use a model with tidal dissipation (and increasing orbital periods) to explain the shift. We also analyzed light curves, spanning 1977--2021, and searched for the expected spin deceleration of Kleopatra. According to our best-fit model, the observed period rate is $\dot P_2 = (1.8\pm 0.1)\cdot 10^{-8}\,{\rm d}\,{\rm d}^{-1}$ and the corresponding time lag $螖t_2 = 42\,{\rm s}$ of tides, for the assumed value of the Love number $k_2 = 0.3$. It is the first detection of tidal evolution for moons orbiting 100-km asteroids. The corresponding dissipation factor $Q$ is comparable with other terrestrial bodies, albeit at a higher loading frequency $2|蠅-n|$. We also predict a secular evolution of the inner moon, $\dot P_1 = 5.0\cdot 10^{-8}$, as well as a spin deceleration of Kleopatra, $\dot P_0 = 1.9\cdot 10^{-12}$. In alternative models, with moons captured in the 3:2 mean-motion resonance or more massive moons, the respective values of $螖t_2$ are a factor of 2--3 lower. Future astrometric observations by direct imaging or occultations should allow to distinguish between these models, which is important for the internal structure and mechanical properties of (216) Kleopatra. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.12702v1-abstract-full').style.display = 'none'; document.getElementById('2110.12702v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 657, A76 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.12669">arXiv:2110.12669</a> <span> [<a href="https://arxiv.org/pdf/2110.12669">pdf</a>, <a href="https://arxiv.org/format/2110.12669">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141598">10.1051/0004-6361/202141598 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neptune's ring arcs from VLT/SPHERE-IRDIS near-infrared observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Souami%2C+D">D. Souami</a>, <a href="/search/astro-ph?searchtype=author&query=Renner%2C+S">S. Renner</a>, <a href="/search/astro-ph?searchtype=author&query=Sicardy%2C+B">B. Sicardy</a>, <a href="/search/astro-ph?searchtype=author&query=Langlois%2C+M">M. Langlois</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Delorme%2C+P">P. Delorme</a>, <a href="/search/astro-ph?searchtype=author&query=Golaszewska%2C+P">P. Golaszewska</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.12669v2-abstract-short" style="display: inline;"> Neptune's incomplete ring arcs have been stable since their discovery in 1984 by stellar occultation. Although these structures should be destroyed within a few months through differential Keplerian motion, imaging data over the past couple of decades has shown that these structures are persistent. We present here the first SPHERE near-infrared observations of Neptune's ring arcs taken at 2.2 $渭$m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.12669v2-abstract-full').style.display = 'inline'; document.getElementById('2110.12669v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.12669v2-abstract-full" style="display: none;"> Neptune's incomplete ring arcs have been stable since their discovery in 1984 by stellar occultation. Although these structures should be destroyed within a few months through differential Keplerian motion, imaging data over the past couple of decades has shown that these structures are persistent. We present here the first SPHERE near-infrared observations of Neptune's ring arcs taken at 2.2 $渭$m (BB-Ks) with the IRDIS camera at the Very Large Telescope in August 2016. The images were aligned using the ephemerides of the satellite Proteus and were suitably co-added to enhance ring and satellite signals. We analyse high-angular resolution near-infrared images of Neptune's ring arcs obtained in 2016 at the ESO VLT-UT3 with the adaptive-optics fed camera SPHERE-IRDIS. We derive here accurate mean motion values for the arcs and the nearby satellite Galatea. The trailing arcs Fraternit茅 and Egalit茅 are stable since they were last observed in 2007. Furthermore, we confirm the fading away of the leading arcs Courage and Libert茅. Finally, we confirm the mismatch between the arcs' position and 42:43 inclined and eccentric corotation resonances with Galatea; thus demonstrating that no 42:43 corotation model works to explain the azimuthal confinement of the arcs' materiel. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.12669v2-abstract-full').style.display = 'none'; document.getElementById('2110.12669v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figure two of which have 2 subfigures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 657, A134 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.11656">arXiv:2110.11656</a> <span> [<a href="https://arxiv.org/pdf/2110.11656">pdf</a>, <a href="https://arxiv.org/format/2110.11656">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202142074">10.1051/0004-6361/202142074 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-filter photometry of Solar System Objects from the SkyMapper Southern Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sergeyev%2C+A+V">A. V. Sergeyev</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Onken%2C+C+A">C. A. Onken</a>, <a href="/search/astro-ph?searchtype=author&query=Devillepoix%2C+H+A+R">H. A. R. Devillepoix</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+C">C. Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+S+-">S. -W. Chang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.11656v1-abstract-short" style="display: inline;"> Context. The populations of small bodies of the Solar System (asteroids, comets, Kuiper Belt objects) are used to constrain the origin and evolution of the Solar System. Both their orbital distribution and composition distribution are required to track the dynamical pathway from their regions of formation to their current locations. Aims. We aim at increasing the sample of Solar System objects (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.11656v1-abstract-full').style.display = 'inline'; document.getElementById('2110.11656v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.11656v1-abstract-full" style="display: none;"> Context. The populations of small bodies of the Solar System (asteroids, comets, Kuiper Belt objects) are used to constrain the origin and evolution of the Solar System. Both their orbital distribution and composition distribution are required to track the dynamical pathway from their regions of formation to their current locations. Aims. We aim at increasing the sample of Solar System objects (SSOs) that have multi-filter photometry and compositional taxonomy. Methods. We search for moving objects in the SkyMapper Southern Survey. We use the predicted SSO positions to extract photometry and astrometry from the SkyMapper frames. We then apply a suite of filters to clean the catalog for false-positive detections. We finally use the near-simultaneous photometry to assign a taxonomic class to objects. Results. We release a catalog of 880,528 individual observations, consisting of 205,515 known and unique SSOs. The catalog completeness is estimated to be about 97% down to V=18 mag and the purity to be above 95% for known SSOs. The near-simultaneous photometry provides either three, two, or a single color that we use to classify 117,356 SSOs with a scheme consistent with the widely used Bus-DeMeo taxonomy. Conclusions. The present catalog contributes significantly to the sample of asteroids with known surface properties (about 40% of main-belt asteroids down to an absolute magnitude of 16). We will release more observations of SSOs with future SkyMapper data releases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.11656v1-abstract-full').style.display = 'none'; document.getElementById('2110.11656v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 22 figures, 13 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 658, A109 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.07207">arXiv:2108.07207</a> <span> [<a href="https://arxiv.org/pdf/2108.07207">pdf</a>, <a href="https://arxiv.org/format/2108.07207">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140874">10.1051/0004-6361/202140874 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> (216) Kleopatra, a low density critically rotating M-type asteroid </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marchis%2C+F">F. Marchis</a>, <a href="/search/astro-ph?searchtype=author&query=Jorda%2C+L">L. Jorda</a>, <a href="/search/astro-ph?searchtype=author&query=Vernazza%2C+P">P. Vernazza</a>, <a href="/search/astro-ph?searchtype=author&query=Bro%C5%BE%2C+M">M. Bro啪</a>, <a href="/search/astro-ph?searchtype=author&query=Hanu%C5%A1%2C+J">J. Hanu拧</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrais%2C+M">M. Ferrais</a>, <a href="/search/astro-ph?searchtype=author&query=Vachier%2C+F">F. Vachier</a>, <a href="/search/astro-ph?searchtype=author&query=Rambaux%2C+N">N. Rambaux</a>, <a href="/search/astro-ph?searchtype=author&query=Marsset%2C+M">M. Marsset</a>, <a href="/search/astro-ph?searchtype=author&query=Viikinkoski%2C+M">M. Viikinkoski</a>, <a href="/search/astro-ph?searchtype=author&query=Jehin%2C+E">E. Jehin</a>, <a href="/search/astro-ph?searchtype=author&query=Benseguane%2C+S">S. Benseguane</a>, <a href="/search/astro-ph?searchtype=author&query=Podlewska-Gaca%2C+E">E. Podlewska-Gaca</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Drouard%2C+A">A. Drouard</a>, <a href="/search/astro-ph?searchtype=author&query=Fauvaud%2C+S">S. Fauvaud</a>, <a href="/search/astro-ph?searchtype=author&query=Birlan%2C+M">M. Birlan</a>, <a href="/search/astro-ph?searchtype=author&query=Berthier%2C+J">J. Berthier</a>, <a href="/search/astro-ph?searchtype=author&query=Bartczak%2C+P">P. Bartczak</a>, <a href="/search/astro-ph?searchtype=author&query=Dumas%2C+C">C. Dumas</a>, <a href="/search/astro-ph?searchtype=author&query=Dudzinski%2C+G">G. Dudzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Durech%2C+J">J. Durech</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo-Rogez%2C+J">J. Castillo-Rogez</a>, <a href="/search/astro-ph?searchtype=author&query=Cipriani%2C+F">F. Cipriani</a>, <a href="/search/astro-ph?searchtype=author&query=Colas%2C+F">F. Colas</a> , et al. (14 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.07207v1-abstract-short" style="display: inline;"> Context. The recent estimates of the 3D shape of the M/Xe-type triple asteroid system (216) Kleopatra indicated a density of 5 g.cm$^{-3}$. Such a high density implies a high metal content and a low porosity which is not easy to reconcile with its peculiar dumbbell shape. Aims. Given the unprecedented angular resolution of the VLT/SPHERE/ZIMPOL camera, we aim to constrain the mass and the shape of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.07207v1-abstract-full').style.display = 'inline'; document.getElementById('2108.07207v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.07207v1-abstract-full" style="display: none;"> Context. The recent estimates of the 3D shape of the M/Xe-type triple asteroid system (216) Kleopatra indicated a density of 5 g.cm$^{-3}$. Such a high density implies a high metal content and a low porosity which is not easy to reconcile with its peculiar dumbbell shape. Aims. Given the unprecedented angular resolution of the VLT/SPHERE/ZIMPOL camera, we aim to constrain the mass and the shape of Kleopatra with high accuracy, hence its density. Methods. We combined our new VLT/SPHERE observations of Kleopatra recorded in 2017 and 2018 with archival data, as well as lightcurve, occultation, and delay-Doppler images, to derive its 3D shape model using two different algorithms (ADAM, MPCD). Furthermore, an N-body dynamical model allowed us to retrieve the orbital elements of the two moons as explained in the accompanying paper. Results. The shape of Kleopatra is very close to an equilibrium dumbbell figure with two lobes and a thick neck. Its volume equivalent diameter (118.75$\pm$1.40) km and mass (2.97$\pm$0.32) 10$^{18}$ kg imply a bulk density of (3.38$\pm$0.50) g cm$^{-3}$. Such a low density for a supposedly metal-rich body indicates a substantial porosity within the primary. This porous structure along with its near-equilibrium shape is compatible with a formation scenario including a giant impact followed by reaccumulation. Kleopatra's current rotation period and dumbbell shape imply that it is in a critically rotating state. The low effective gravity along the equator of the body, together with the equatorial orbits of the moons and possibly rubble-pile structure, opens the possibility that the moons formed via mass shedding. Conclusions. Kleopatra is a puzzling multiple system due to the unique characteristics of the primary. It deserves particular attention in the future, with the Extremely Large Telescopes and possibly a dedicated space mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.07207v1-abstract-full').style.display = 'none'; document.getElementById('2108.07207v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 653, A57 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.05749">arXiv:2108.05749</a> <span> [<a href="https://arxiv.org/pdf/2108.05749">pdf</a>, <a href="https://arxiv.org/format/2108.05749">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140430">10.1051/0004-6361/202140430 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A million asteroid observations in the Sloan Digital Sky Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sergeyev%2C+A+V">A. V. Sergeyev</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.05749v1-abstract-short" style="display: inline;"> Context. The populations of small bodies of the Solar System (asteroids, comets, Kuiper-Belt objects) are used to constrain the origin and evolution of the Solar System. Both their orbital distribution and composition distribution are required to track the dynamical pathway from their regions of formation to their current locations. Aims. We aim at increasing the sample of Solar System objects t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.05749v1-abstract-full').style.display = 'inline'; document.getElementById('2108.05749v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.05749v1-abstract-full" style="display: none;"> Context. The populations of small bodies of the Solar System (asteroids, comets, Kuiper-Belt objects) are used to constrain the origin and evolution of the Solar System. Both their orbital distribution and composition distribution are required to track the dynamical pathway from their regions of formation to their current locations. Aims. We aim at increasing the sample of Solar System objects that have multi-filter photometry and compositional taxonomy. Methods. We search for moving objects in the archive of the Sloan Digital Sky Survey. We attempt at maximizing the number of detections by using loose constraints on the extraction. We then apply a suite of filters to remove false-positive detections (stars or galaxies) and mark out spurious photometry and astrometry. Results. We release a catalog of 1 542 522 entries, consisting of 1 036 322 observations of 379 714 known and unique SSOs together with 506 200 observations of moving sources not linked with any known SSOs. The catalog completeness is estimated to be about 95% and the purity to be above 95% for known SSOs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.05749v1-abstract-full').style.display = 'none'; document.getElementById('2108.05749v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 13 figures. The catalog is available at the CDS via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/652/A59</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A Volume 652 August 2021, A59 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.09134">arXiv:2105.09134</a> <span> [<a href="https://arxiv.org/pdf/2105.09134">pdf</a>, <a href="https://arxiv.org/ps/2105.09134">ps</a>, <a href="https://arxiv.org/format/2105.09134">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140901">10.1051/0004-6361/202140901 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An advanced multipole model for (216) Kleopatra triple system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bro%C5%BE%2C+M">M. Bro啪</a>, <a href="/search/astro-ph?searchtype=author&query=Marchis%2C+F">F. Marchis</a>, <a href="/search/astro-ph?searchtype=author&query=Jorda%2C+L">L. Jorda</a>, <a href="/search/astro-ph?searchtype=author&query=Hanu%C5%A1%2C+J">J. Hanu拧</a>, <a href="/search/astro-ph?searchtype=author&query=Vernazza%2C+P">P. Vernazza</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrais%2C+M">M. Ferrais</a>, <a href="/search/astro-ph?searchtype=author&query=Vachier%2C+F">F. Vachier</a>, <a href="/search/astro-ph?searchtype=author&query=Rambaux%2C+N">N. Rambaux</a>, <a href="/search/astro-ph?searchtype=author&query=Marsset%2C+M">M. Marsset</a>, <a href="/search/astro-ph?searchtype=author&query=Viikinkoski%2C+M">M. Viikinkoski</a>, <a href="/search/astro-ph?searchtype=author&query=Jehin%2C+E">E. Jehin</a>, <a href="/search/astro-ph?searchtype=author&query=Benseguane%2C+S">S. Benseguane</a>, <a href="/search/astro-ph?searchtype=author&query=Podlewska-Gaca%2C+E">E. Podlewska-Gaca</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Drouard%2C+A">A. Drouard</a>, <a href="/search/astro-ph?searchtype=author&query=Fauvaud%2C+S">S. Fauvaud</a>, <a href="/search/astro-ph?searchtype=author&query=Birlan%2C+M">M. Birlan</a>, <a href="/search/astro-ph?searchtype=author&query=Berthier%2C+J">J. Berthier</a>, <a href="/search/astro-ph?searchtype=author&query=Bartczak%2C+P">P. Bartczak</a>, <a href="/search/astro-ph?searchtype=author&query=Dumas%2C+C">C. Dumas</a>, <a href="/search/astro-ph?searchtype=author&query=Dudzi%C5%84ski%2C+G">G. Dudzi艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=%C4%8Eurech%2C+J">J. 膸urech</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo-Rogez%2C+J">J. Castillo-Rogez</a>, <a href="/search/astro-ph?searchtype=author&query=Cipriani%2C+F">F. Cipriani</a>, <a href="/search/astro-ph?searchtype=author&query=Colas%2C+F">F. Colas</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.09134v1-abstract-short" style="display: inline;"> To interpret adaptive-optics observations of (216) Kleopatra, we need to describe an evolution of multiple moons, orbiting an extremely irregular body and including their mutual interactions. Such orbits are generally non-Keplerian and orbital elements are not constants. Consequently, we use a modified $N$-body integrator, which was significantly extended to include the multipole expansion of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09134v1-abstract-full').style.display = 'inline'; document.getElementById('2105.09134v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.09134v1-abstract-full" style="display: none;"> To interpret adaptive-optics observations of (216) Kleopatra, we need to describe an evolution of multiple moons, orbiting an extremely irregular body and including their mutual interactions. Such orbits are generally non-Keplerian and orbital elements are not constants. Consequently, we use a modified $N$-body integrator, which was significantly extended to include the multipole expansion of the gravitational field up to the order $\ell = 10$. Its convergence was verified against the `brute-force' algorithm. We computed the coefficients $C_{\ell m},S_{\!\ell m}$ for Kleopatra's shape, assuming a~constant bulk density. For solar-system applications, it was also necessary to implement a variable distance and geometry of observations. Our $蠂^2$ metric then accounts for the absolute astrometry, the relative astrometry (2nd moon with respect to 1st), angular velocities, and also silhouettes, constraining the pole orientation. This allowed us to derive the orbital elements of Kleopatra's two moons. Using both archival astrometric data and new VLT/SPHERE observations (ESO LP 199.C-0074), we were able to identify the true periods of the moons, $P_1 = (1.822359\pm0.004156)\,{\rm d}$, $P_2 = (2.745820\pm0.004820)\,{\rm d}$. They orbit very close to the 3:2 mean-motion resonance, but their osculating eccentricities are too small compared to other perturbations (multipole, mutual), so that regular librations of the critical argument are not present. The resulting mass of Kleopatra, $m_1 = (1.49\pm0.16)\cdot10^{-12}\,M_\odot$ or $2.97\cdot10^{18}\,{\rm kg}$, is significantly lower than previously thought. An implication explained in the accompanying paper (Marchis et al.) is that (216) Kleopatra is a critically rotating body. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09134v1-abstract-full').style.display = 'none'; document.getElementById('2105.09134v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 653, A56 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.06349">arXiv:2103.06349</a> <span> [<a href="https://arxiv.org/pdf/2103.06349">pdf</a>, <a href="https://arxiv.org/format/2103.06349">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140342">10.1051/0004-6361/202140342 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence for differentiation of the most primitive small bodies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Vernazza%2C+P">P. Vernazza</a>, <a href="/search/astro-ph?searchtype=author&query=Vachier%2C+F">F. Vachier</a>, <a href="/search/astro-ph?searchtype=author&query=Neveu%2C+M">M. Neveu</a>, <a href="/search/astro-ph?searchtype=author&query=Hanus%2C+J+B+J">J. Berthier J. Hanus</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrais%2C+M">M. Ferrais</a>, <a href="/search/astro-ph?searchtype=author&query=Jorda%2C+L">L. Jorda</a>, <a href="/search/astro-ph?searchtype=author&query=Marsset%2C+M">M. Marsset</a>, <a href="/search/astro-ph?searchtype=author&query=Viikinkoski%2C+M">M. Viikinkoski</a>, <a href="/search/astro-ph?searchtype=author&query=Bartczak%2C+P">P. Bartczak</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+R">R. Behrend</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhaldoun%2C+Z">Z. Benkhaldoun</a>, <a href="/search/astro-ph?searchtype=author&query=Birlan%2C+M">M. Birlan</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo-Rogez%2C+J">J. Castillo-Rogez</a>, <a href="/search/astro-ph?searchtype=author&query=Cipriani%2C+F">F. Cipriani</a>, <a href="/search/astro-ph?searchtype=author&query=Colas%2C+F">F. Colas</a>, <a href="/search/astro-ph?searchtype=author&query=Drouard%2C+A">A. Drouard</a>, <a href="/search/astro-ph?searchtype=author&query=Dudzinski%2C+G+P">G. P. Dudzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Desmars%2C+J">J. Desmars</a>, <a href="/search/astro-ph?searchtype=author&query=Dumas%2C+C">C. Dumas</a>, <a href="/search/astro-ph?searchtype=author&query=Durech%2C+J">J. Durech</a>, <a href="/search/astro-ph?searchtype=author&query=Fetick%2C+R">R. Fetick</a>, <a href="/search/astro-ph?searchtype=author&query=Fusco%2C+T">T. Fusco</a>, <a href="/search/astro-ph?searchtype=author&query=Grice%2C+J">J. Grice</a>, <a href="/search/astro-ph?searchtype=author&query=Jehin%2C+E">E. Jehin</a> , et al. (18 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.06349v1-abstract-short" style="display: inline;"> Dynamical models of Solar System evolution have suggested that P-/D-type volatile-rich asteroids formed in the outer Solar System and may be genetically related to the Jupiter Trojans, the comets and small KBOs. Indeed, their spectral properties resemble that of anhydrous cometary dust. High-angular-resolution images of P-type asteroid (87) Sylvia with VLT/SPHERE were used to reconstruct its 3D sh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.06349v1-abstract-full').style.display = 'inline'; document.getElementById('2103.06349v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.06349v1-abstract-full" style="display: none;"> Dynamical models of Solar System evolution have suggested that P-/D-type volatile-rich asteroids formed in the outer Solar System and may be genetically related to the Jupiter Trojans, the comets and small KBOs. Indeed, their spectral properties resemble that of anhydrous cometary dust. High-angular-resolution images of P-type asteroid (87) Sylvia with VLT/SPHERE were used to reconstruct its 3D shape, and to study the dynamics of its two satellites. We also model Sylvia's thermal evolution. The shape of Sylvia appears flattened and elongated. We derive a volume-equivalent diameter of 271 +/- 5 km, and a low density of 1378 +/- 45 kg.m-3. The two satellites orbit Sylvia on circular, equatorial orbits. The oblateness of Sylvia should imply a detectable nodal precession which contrasts with the fully-Keplerian dynamics of the satellites. This reveals an inhomogeneous internal structure, suggesting that Sylvia is differentiated. Sylvia's low density and differentiated interior can be explained by partial melting and mass redistribution through water percolation. The outer shell would be composed of material similar to interplanetary dust particles (IDPs) and the core similar to aqueously altered IDPs or carbonaceous chondrite meteorites such as the Tagish Lake meteorite. Numerical simulations of the thermal evolution of Sylvia show that for a body of such size, partial melting was unavoidable due to the decay of long-lived radionuclides. In addition, we show that bodies as small as 130-150 km in diameter should have followed a similar thermal evolution, while smaller objects, such as comets and the KBO Arrokoth, must have remained pristine, in agreement with in situ observations of these bodies. NASA Lucy mission target (617) Patroclus (diameter~140 km) may, however, be differentiated. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.06349v1-abstract-full').style.display = 'none'; document.getElementById('2103.06349v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 650, A129 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.05811">arXiv:2101.05811</a> <span> [<a href="https://arxiv.org/pdf/2101.05811">pdf</a>, <a href="https://arxiv.org/format/2101.05811">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202039714">10.1051/0004-6361/202039714 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: The Galactic anticentre </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Antoja%2C+T">T. Antoja</a>, <a href="/search/astro-ph?searchtype=author&query=McMillan%2C+P">P. McMillan</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">G. Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+P">P. Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Helmi%2C+A">A. Helmi</a>, <a href="/search/astro-ph?searchtype=author&query=Balbinot%2C+E">E. Balbinot</a>, <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Figueras%2C+F">F. Figueras</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Khanna%2C+S">S. Khanna</a>, <a href="/search/astro-ph?searchtype=author&query=Romero-Gomez%2C+M">M. Romero-Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Seabroke%2C+G">G. Seabroke</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+F">F. Jansen</a> , et al. (395 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.05811v2-abstract-short" style="display: inline;"> We aim to demonstrate the scientific potential of the Gaia Early Data Release 3 (EDR3) for the study of the Milky Way structure and evolution. We used astrometric positions, proper motions, parallaxes, and photometry from EDR3 to select different populations and components and to calculate the distances and velocities in the direction of the anticentre. We explore the disturbances of the current d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05811v2-abstract-full').style.display = 'inline'; document.getElementById('2101.05811v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.05811v2-abstract-full" style="display: none;"> We aim to demonstrate the scientific potential of the Gaia Early Data Release 3 (EDR3) for the study of the Milky Way structure and evolution. We used astrometric positions, proper motions, parallaxes, and photometry from EDR3 to select different populations and components and to calculate the distances and velocities in the direction of the anticentre. We explore the disturbances of the current disc, the spatial and kinematical distributions of early accreted versus in-situ stars, the structures in the outer parts of the disc, and the orbits of open clusters Berkeley 29 and Saurer 1. We find that: i) the dynamics of the Galactic disc are very complex with vertical asymmetries, and new correlations, including a bimodality with disc stars with large angular momentum moving vertically upwards from below the plane, and disc stars with slightly lower angular momentum moving preferentially downwards; ii) we resolve the kinematic substructure (diagonal ridges) in the outer parts of the disc for the first time; iii) the red sequence that has been associated with the proto-Galactic disc that was present at the time of the merger with Gaia-Enceladus-Sausage is currently radially concentrated up to around 14 kpc, while the blue sequence that has been associated with debris of the satellite extends beyond that; iv) there are density structures in the outer disc, both above and below the plane, most probably related to Monoceros, the Anticentre Stream, and TriAnd, for which the Gaia data allow an exhaustive selection of candidate member stars and dynamical study; and v) the open clusters Berkeley~29 and Saurer~1, despite being located at large distances from the Galactic centre, are on nearly circular disc-like orbits. We demonstrate how, once again, the Gaia are crucial for our understanding of the different pieces of our Galaxy and their connection to its global structure and history. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05811v2-abstract-full').style.display = 'none'; document.getElementById('2101.05811v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Gaia EDR3 performance verification paper, version 2 closer to published version in A&A, complete list of authors</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A8 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02061">arXiv:2012.02061</a> <span> [<a href="https://arxiv.org/pdf/2012.02061">pdf</a>, <a href="https://arxiv.org/format/2012.02061">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202039498">10.1051/0004-6361/202039498 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: The Gaia Catalogue of Nearby Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R+L">R. L. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Sarro%2C+L+M">L. M. Sarro</a>, <a href="/search/astro-ph?searchtype=author&query=Rybizki%2C+J">J. Rybizki</a>, <a href="/search/astro-ph?searchtype=author&query=Reyl%C3%A9%2C+C">C. Reyl茅</a>, <a href="/search/astro-ph?searchtype=author&query=Robin%2C+A+C">A. C. Robin</a>, <a href="/search/astro-ph?searchtype=author&query=Hambly%2C+N+C">N. C. Hambly</a>, <a href="/search/astro-ph?searchtype=author&query=Abbas%2C+U">U. Abbas</a>, <a href="/search/astro-ph?searchtype=author&query=Barstow%2C+M+A">M. A. Barstow</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Bucciarelli%2C+B">B. Bucciarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+J+M">J. M. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+W+J">W. J. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">S. T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Masana%2C+E">E. Masana</a>, <a href="/search/astro-ph?searchtype=author&query=Michalik%2C+D">D. Michalik</a>, <a href="/search/astro-ph?searchtype=author&query=Sahlmann%2C+J">J. Sahlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a> , et al. (398 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.02061v1-abstract-short" style="display: inline;"> We produce a clean and well-characterised catalogue of objects within 100\,pc of the Sun from the \G\ Early Data Release 3. We characterise the catalogue through comparisons to the full data release, external catalogues, and simulations. We carry out a first analysis of the science that is possible with this sample to demonstrate its potential and best practices for its use. The selection of obj… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02061v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02061v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02061v1-abstract-full" style="display: none;"> We produce a clean and well-characterised catalogue of objects within 100\,pc of the Sun from the \G\ Early Data Release 3. We characterise the catalogue through comparisons to the full data release, external catalogues, and simulations. We carry out a first analysis of the science that is possible with this sample to demonstrate its potential and best practices for its use. The selection of objects within 100\,pc from the full catalogue used selected training sets, machine-learning procedures, astrometric quantities, and solution quality indicators to determine a probability that the astrometric solution is reliable. The training set construction exploited the astrometric data, quality flags, and external photometry. For all candidates we calculated distance posterior probability densities using Bayesian procedures and mock catalogues to define priors. Any object with reliable astrometry and a non-zero probability of being within 100\,pc is included in the catalogue. We have produced a catalogue of \NFINAL\ objects that we estimate contains at least 92\% of stars of stellar type M9 within 100\,pc of the Sun. We estimate that 9\% of the stars in this catalogue probably lie outside 100\,pc, but when the distance probability function is used, a correct treatment of this contamination is possible. We produced luminosity functions with a high signal-to-noise ratio for the main-sequence stars, giants, and white dwarfs. We examined in detail the Hyades cluster, the white dwarf population, and wide-binary systems and produced candidate lists for all three samples. We detected local manifestations of several streams, superclusters, and halo objects, in which we identified 12 members of \G\ Enceladus. We present the first direct parallaxes of five objects in multiple systems within 10\,pc of the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02061v1-abstract-full').style.display = 'none'; document.getElementById('2012.02061v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">45 Pages, 39 figures in main part and 18 in appendix, tables on CDS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A6 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02036">arXiv:2012.02036</a> <span> [<a href="https://arxiv.org/pdf/2012.02036">pdf</a>, <a href="https://arxiv.org/format/2012.02036">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202039734">10.1051/0004-6361/202039734 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: Acceleration of the solar system from Gaia astrometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+U">U. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=McMillan%2C+P+J">P. J. McMillan</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">J. Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+D">D. Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Lerate%2C+M">M. Ramos-Lerate</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Bombrun%2C+A">A. Bombrun</a>, <a href="/search/astro-ph?searchtype=author&query=de+Torres%2C+A">A. de Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Gerlach%2C+E">E. Gerlach</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+R">R. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hilger%2C+T">T. Hilger</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U">U. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=Steidelm%C3%BCller%2C+H">H. Steidelm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Stephenson%2C+C+A">C. A. Stephenson</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a> , et al. (392 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.02036v1-abstract-short" style="display: inline;"> Context. Gaia Early Data Release 3 (Gaia EDR3) provides accurate astrometry for about 1.6 million compact (QSO-like) extragalactic sources, 1.2 million of which have the best-quality five-parameter astrometric solutions. Aims. The proper motions of QSO-like sources are used to reveal a systematic pattern due to the acceleration of the solar system barycentre with respect to the rest frame of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02036v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02036v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02036v1-abstract-full" style="display: none;"> Context. Gaia Early Data Release 3 (Gaia EDR3) provides accurate astrometry for about 1.6 million compact (QSO-like) extragalactic sources, 1.2 million of which have the best-quality five-parameter astrometric solutions. Aims. The proper motions of QSO-like sources are used to reveal a systematic pattern due to the acceleration of the solar system barycentre with respect to the rest frame of the Universe. Apart from being an important scientific result by itself, the acceleration measured in this way is a good quality indicator of the Gaia astrometric solution. Methods. The effect of the acceleration is obtained as a part of the general expansion of the vector field of proper motions in Vector Spherical Harmonics (VSH). Various versions of the VSH fit and various subsets of the sources are tried and compared to get the most consistent result and a realistic estimate of its uncertainty. Additional tests with the Gaia astrometric solution are used to get a better idea on possible systematic errors in the estimate. Results. Our best estimate of the acceleration based on Gaia EDR3 is $(2.32 \pm 0.16) \times 10^{-10}$ m s${}^{-2}$ (or $7.33 \pm 0.51$ km s$^{-1}$ Myr${}^{-1}$) towards $伪= 269.1^\circ \pm 5.4^\circ$, $未= -31.6^\circ \pm 4.1^\circ$, corresponding to a proper motion amplitude of $5.05 \pm 0.35$ $渭$as yr${}^{-1}$. This is in good agreement with the acceleration expected from current models of the Galactic gravitational potential. We expect that future Gaia data releases will provide estimates of the acceleration with uncertainties substantially below 0.1 $渭$as yr${}^{-1}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02036v1-abstract-full').style.display = 'none'; document.getElementById('2012.02036v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A&A, accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A9 (2021) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Carry%2C+B&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Carry%2C+B&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Carry%2C+B&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Carry%2C+B&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

CINXE.COM

Search | arXiv e-print repository